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Liu Q, Tan S, Zou X, Liu P, Yu S. Wavelength-Dependent Dynamics of the O( 1D 2) Channel in the 1Δ u State Photodissociation of CO 2. J Phys Chem A 2024; 128:2989-2996. [PMID: 38572621 DOI: 10.1021/acs.jpca.4c00223] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/05/2024]
Abstract
The wavelength-dependent dynamics of the O(1D2) channel, formed by photoexcitation of CO2 to the 1Δu state at 143.53-153.03 nm, is investigated by using the time-sliced velocity-mapped ion imaging method. The measured ionic peaks of the O(1D2) images are analyzed to determine the total kinetic energy release (TKER) spectra and image anisotropy parameters. The structures observed in the TKER spectra can be directly assigned to the ro-vibrational state distributions of the counter CO photofragments. Compared to those observed at 157 and 155 nm, the highly rotationally excited CO photofragments still obviously appear in v = 0 and 1, but the fraction of rotational excitations is significantly reduced. Conversely, the CO photofragments exhibit substantially higher vibrational excitations, implying that the nearly linear 21A' state also contributes to dissociation in addition to the bend configuration. The image anisotropy parameters display an extremely slow decreasing trend with an increase of the CO ro-vibrational state besides those for the highest ro-vibrationally excited CO photofragments. Nevertheless, the nonaxial recoil effect, suggested in previous photodissociation studies of CO2 and other triatomic molecular systems, is still appropriate to explain the observations of internal energy dependences of image anisotropy parameters.
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Affiliation(s)
- Qian Liu
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang, P. R. China
| | - Sha Tan
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang, P. R. China
| | - Xiaolan Zou
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang, P. R. China
| | - Peng Liu
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang, P. R. China
| | - Shengrui Yu
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang, P. R. China
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2
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Jones GH, Snodgrass C, Tubiana C, Küppers M, Kawakita H, Lara LM, Agarwal J, André N, Attree N, Auster U, Bagnulo S, Bannister M, Beth A, Bowles N, Coates A, Colangeli L, Corral van Damme C, Da Deppo V, De Keyser J, Della Corte V, Edberg N, El-Maarry MR, Faggi S, Fulle M, Funase R, Galand M, Goetz C, Groussin O, Guilbert-Lepoutre A, Henri P, Kasahara S, Kereszturi A, Kidger M, Knight M, Kokotanekova R, Kolmasova I, Kossacki K, Kührt E, Kwon Y, La Forgia F, Levasseur-Regourd AC, Lippi M, Longobardo A, Marschall R, Morawski M, Muñoz O, Näsilä A, Nilsson H, Opitom C, Pajusalu M, Pommerol A, Prech L, Rando N, Ratti F, Rothkaehl H, Rotundi A, Rubin M, Sakatani N, Sánchez JP, Simon Wedlund C, Stankov A, Thomas N, Toth I, Villanueva G, Vincent JB, Volwerk M, Wurz P, Wielders A, Yoshioka K, Aleksiejuk K, Alvarez F, Amoros C, Aslam S, Atamaniuk B, Baran J, Barciński T, Beck T, Behnke T, Berglund M, Bertini I, Bieda M, Binczyk P, Busch MD, Cacovean A, Capria MT, Carr C, Castro Marín JM, Ceriotti M, Chioetto P, Chuchra-Konrad A, Cocola L, Colin F, Crews C, Cripps V, Cupido E, Dassatti A, Davidsson BJR, De Roche T, Deca J, Del Togno S, Dhooghe F, Donaldson Hanna K, Eriksson A, Fedorov A, Fernández-Valenzuela E, Ferretti S, Floriot J, Frassetto F, Fredriksson J, Garnier P, Gaweł D, Génot V, Gerber T, Glassmeier KH, Granvik M, Grison B, Gunell H, Hachemi T, Hagen C, Hajra R, Harada Y, Hasiba J, Haslebacher N, Herranz De La Revilla ML, Hestroffer D, Hewagama T, Holt C, Hviid S, Iakubivskyi I, Inno L, Irwin P, Ivanovski S, Jansky J, Jernej I, Jeszenszky H, Jimenéz J, Jorda L, Kama M, Kameda S, Kelley MSP, Klepacki K, Kohout T, Kojima H, Kowalski T, Kuwabara M, Ladno M, Laky G, Lammer H, Lan R, Lavraud B, Lazzarin M, Le Duff O, Lee QM, Lesniak C, Lewis Z, Lin ZY, Lister T, Lowry S, Magnes W, Markkanen J, Martinez Navajas I, Martins Z, Matsuoka A, Matyjasiak B, Mazelle C, Mazzotta Epifani E, Meier M, Michaelis H, Micheli M, Migliorini A, Millet AL, Moreno F, Mottola S, Moutounaick B, Muinonen K, Müller DR, Murakami G, Murata N, Myszka K, Nakajima S, Nemeth Z, Nikolajev A, Nordera S, Ohlsson D, Olesk A, Ottacher H, Ozaki N, Oziol C, Patel M, Savio Paul A, Penttilä A, Pernechele C, Peterson J, Petraglio E, Piccirillo AM, Plaschke F, Polak S, Postberg F, Proosa H, Protopapa S, Puccio W, Ranvier S, Raymond S, Richter I, Rieder M, Rigamonti R, Ruiz Rodriguez I, Santolik O, Sasaki T, Schrödter R, Shirley K, Slavinskis A, Sodor B, Soucek J, Stephenson P, Stöckli L, Szewczyk P, Troznai G, Uhlir L, Usami N, Valavanoglou A, Vaverka J, Wang W, Wang XD, Wattieaux G, Wieser M, Wolf S, Yano H, Yoshikawa I, Zakharov V, Zawistowski T, Zuppella P, Rinaldi G, Ji H. The Comet Interceptor Mission. SPACE SCIENCE REVIEWS 2024; 220:9. [PMID: 38282745 PMCID: PMC10808369 DOI: 10.1007/s11214-023-01035-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/14/2022] [Accepted: 11/29/2023] [Indexed: 01/30/2024]
Abstract
Here we describe the novel, multi-point Comet Interceptor mission. It is dedicated to the exploration of a little-processed long-period comet, possibly entering the inner Solar System for the first time, or to encounter an interstellar object originating at another star. The objectives of the mission are to address the following questions: What are the surface composition, shape, morphology, and structure of the target object? What is the composition of the gas and dust in the coma, its connection to the nucleus, and the nature of its interaction with the solar wind? The mission was proposed to the European Space Agency in 2018, and formally adopted by the agency in June 2022, for launch in 2029 together with the Ariel mission. Comet Interceptor will take advantage of the opportunity presented by ESA's F-Class call for fast, flexible, low-cost missions to which it was proposed. The call required a launch to a halo orbit around the Sun-Earth L2 point. The mission can take advantage of this placement to wait for the discovery of a suitable comet reachable with its minimum Δ V capability of 600 ms - 1 . Comet Interceptor will be unique in encountering and studying, at a nominal closest approach distance of 1000 km, a comet that represents a near-pristine sample of material from the formation of the Solar System. It will also add a capability that no previous cometary mission has had, which is to deploy two sub-probes - B1, provided by the Japanese space agency, JAXA, and B2 - that will follow different trajectories through the coma. While the main probe passes at a nominal 1000 km distance, probes B1 and B2 will follow different chords through the coma at distances of 850 km and 400 km, respectively. The result will be unique, simultaneous, spatially resolved information of the 3-dimensional properties of the target comet and its interaction with the space environment. We present the mission's science background leading to these objectives, as well as an overview of the scientific instruments, mission design, and schedule.
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Affiliation(s)
- Geraint H. Jones
- Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, UK
- The Centre for Planetary Sciences at UCL/Birkbeck, London, UK
| | | | | | - Michael Küppers
- European Space Agency (ESA), European Space Astronomy Centre (ESAC), Madrid, Spain
| | - Hideyo Kawakita
- Koyama Astronomical Observatory, Kyoto Sangyo University, Kyoto, Japan
| | - Luisa M. Lara
- Instituto de Astrofisica de Andalucía – CSIC, Granada, Spain
| | - Jessica Agarwal
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | - Nicolas André
- IRAP, CNRS, University Toulouse 3, CNES, Toulouse, France
| | - Nicholas Attree
- Instituto de Astrofisica de Andalucía – CSIC, Granada, Spain
| | - Uli Auster
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | | | | | - Arnaud Beth
- Department of Physics, Imperial College London, London, UK
| | - Neil Bowles
- Department of Physics, University of Oxford, Oxford, UK
| | - Andrew Coates
- Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, UK
- The Centre for Planetary Sciences at UCL/Birkbeck, London, UK
| | | | | | - Vania Da Deppo
- CNR-Institute for Photonics and Nanotechnologies, Padova, Italy
| | - Johan De Keyser
- Royal Belgian Institute of Space Aeronomy, Brussels, Belgium
| | | | - Niklas Edberg
- Swedish Institute of Space Physics, Uppsala/Kiruna, Sweden
| | - Mohamed Ramy El-Maarry
- Space and Planetary Science Center and Department of Earth Sciences, Khalifa University, Abu Dhabi, United Arab Emirates
| | - Sara Faggi
- NASA Goddard Space Flight Center, Greenbelt, USA
| | - Marco Fulle
- INAF – Osservatorio Astronomico di Trieste, Trieste, Italy
| | - Ryu Funase
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | - Marina Galand
- Department of Physics, Imperial College London, London, UK
| | | | - Olivier Groussin
- Laboratoire d’Astrophysique de Marseille, Aix-Marseille Université, CNRS, Marseille, France
| | | | - Pierre Henri
- Laboratoire Lagrange, CNRS, OCA, Université Côte d’Azur, and LPC2E, CNRS, Université d’Orléans, CNES, Orléans, France
| | | | - Akos Kereszturi
- Konkoly Astronomical Institute, Research Centre for Astronomy and Earth Sciences, HUN-REN, Budapest, Hungary
| | - Mark Kidger
- European Space Agency (ESA), European Space Astronomy Centre (ESAC), Madrid, Spain
| | | | - Rosita Kokotanekova
- Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Sofia, Bulgaria
| | - Ivana Kolmasova
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | | | - Ekkehard Kührt
- DLR, Institute of Optical Sensor Systems, Berlin, Germany
| | - Yuna Kwon
- Caltech/IPAC, 1200 E California Blvd, MC 100-22 Pasadena, CA 91125, USA
| | | | | | - Manuela Lippi
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | | | - Raphael Marschall
- CNRS, Laboratoire J.-L. Lagrange, Observatoire de la Côte d’Azur, Nice, France
| | - Marek Morawski
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | - Olga Muñoz
- Instituto de Astrofisica de Andalucía – CSIC, Granada, Spain
| | - Antti Näsilä
- VTT Technical Research Centre of Finland Ltd, Espoo, Finland
| | - Hans Nilsson
- Swedish Institute of Space Physics, Uppsala/Kiruna, Sweden
| | | | | | - Antoine Pommerol
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | | | - Nicola Rando
- European Space Agency, ESTEC, Noordwijk, The Netherlands
| | | | - Hanna Rothkaehl
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | - Alessandra Rotundi
- Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli “Parthenope”, Napoli, Italy
| | - Martin Rubin
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Naoya Sakatani
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | - Joan Pau Sánchez
- Institut Supérieur de l’Aéronautique et de l’Espace, Toulouse, France
| | | | | | - Nicolas Thomas
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Imre Toth
- Konkoly Astronomical Institute, Research Centre for Astronomy and Earth Sciences, HUN-REN, Budapest, Hungary
| | | | | | - Martin Volwerk
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Peter Wurz
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Arno Wielders
- European Space Agency, ESTEC, Noordwijk, The Netherlands
| | | | - Konrad Aleksiejuk
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | | | - Carine Amoros
- IRAP, CNRS, University Toulouse 3, CNES, Toulouse, France
| | - Shahid Aslam
- NASA Goddard Space Flight Center, Greenbelt, USA
| | - Barbara Atamaniuk
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | - Jędrzej Baran
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | - Tomasz Barciński
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | - Thomas Beck
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Thomas Behnke
- DLR Institute of Planetary Research, Berlin, Germany
| | | | - Ivano Bertini
- Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli “Parthenope”, Napoli, Italy
| | | | | | - Martin-Diego Busch
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | | | | | - Chris Carr
- Department of Physics, Imperial College London, London, UK
| | | | | | - Paolo Chioetto
- CNR-Institute for Photonics and Nanotechnologies, Padova, Italy
| | | | - Lorenzo Cocola
- CNR-Institute for Photonics and Nanotechnologies, Padova, Italy
| | - Fabrice Colin
- LPC2E, CNRS, Université d’Orléans, CNES, Orléans, France
| | | | | | | | - Alberto Dassatti
- REDS, School of Management and Engineering Vaud, HES-SO University of Applied Sciences and Arts Western Switzerland, Delémont, Switzerland
| | | | - Thierry De Roche
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Jan Deca
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, USA
| | | | | | | | | | - Andrey Fedorov
- IRAP, CNRS, University Toulouse 3, CNES, Toulouse, France
| | | | - Stefano Ferretti
- Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli “Parthenope”, Napoli, Italy
| | - Johan Floriot
- Laboratoire d’Astrophysique de Marseille, Aix-Marseille Université, CNRS, Marseille, France
| | - Fabio Frassetto
- CNR-Institute for Photonics and Nanotechnologies, Padova, Italy
| | | | | | | | - Vincent Génot
- IRAP, CNRS, University Toulouse 3, CNES, Toulouse, France
| | - Thomas Gerber
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Karl-Heinz Glassmeier
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | - Mikael Granvik
- Department of Physics, University of Helsinki, Helsinki, Finland
- Asteroid Engineering Lab, Luleå University of Technology, Kiruna, Sweden
| | - Benjamin Grison
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | | | | | - Christian Hagen
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | | | | | - Johann Hasiba
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Nico Haslebacher
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | | | - Daniel Hestroffer
- IMCCE, Paris Observatory, Université PSL, CNRS, Sorbonne Université, Univ. Lille, Paris, France
| | | | | | - Stubbe Hviid
- DLR Institute of Planetary Research, Berlin, Germany
| | | | - Laura Inno
- Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli “Parthenope”, Napoli, Italy
| | - Patrick Irwin
- Department of Physics, University of Oxford, Oxford, UK
| | | | - Jiri Jansky
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | - Irmgard Jernej
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Harald Jeszenszky
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Jaime Jimenéz
- Instituto de Astrofisica de Andalucía – CSIC, Granada, Spain
| | - Laurent Jorda
- Laboratoire d’Astrophysique de Marseille, Aix-Marseille Université, CNRS, Marseille, France
| | - Mihkel Kama
- Tartu Observatory, University of Tartu, Tartu, Estonia
- University College London, London, UK
| | | | | | | | - Tomáš Kohout
- Department of Geosciences and Geography, University of Helsinki, Helsinki, Finland
- Institute of Geology of the Czech Academy of Sciences, Prague, Czech Republic
| | - Hirotsugu Kojima
- Research Institute for Sustainable Humanosphere, Kyoto University, Kyoto, Japan
| | - Tomasz Kowalski
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | | | | | - Gunter Laky
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Helmut Lammer
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Radek Lan
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | - Benoit Lavraud
- Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS, Nouvelle-Aquitaine, France
| | - Monica Lazzarin
- Department of Physics and Astronomy, University of Padova, Padova, Italy
| | | | - Qiu-Mei Lee
- IRAP, CNRS, University Toulouse 3, CNES, Toulouse, France
| | | | - Zoe Lewis
- Department of Physics, Imperial College London, London, UK
| | - Zhong-Yi Lin
- Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | | | | | - Werner Magnes
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Johannes Markkanen
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | | | - Zita Martins
- Centro de Química Estrutural, Institute of Molecular Sciences and Department of Chemical Engineering, Instituto Superior Técnico, Universidade de Lisboa, Lisbon, Portugal
| | | | | | | | | | - Mirko Meier
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | | | | | | | | | - Fernando Moreno
- Instituto de Astrofisica de Andalucía – CSIC, Granada, Spain
| | | | | | - Karri Muinonen
- Department of Physics, University of Helsinki, Helsinki, Finland
| | - Daniel R. Müller
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Go Murakami
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | - Naofumi Murata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | | | - Shintaro Nakajima
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | - Zoltan Nemeth
- Wigner Research Centre for Physics, Budapest, Hungary
| | | | - Simone Nordera
- CNR-Institute for Photonics and Nanotechnologies, Padova, Italy
| | - Dan Ohlsson
- Swedish Institute of Space Physics, Uppsala/Kiruna, Sweden
| | - Aire Olesk
- Tartu Observatory, University of Tartu, Tartu, Estonia
| | - Harald Ottacher
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | - Naoya Ozaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | | | | | | | - Antti Penttilä
- Department of Physics, University of Helsinki, Helsinki, Finland
| | | | | | - Enrico Petraglio
- REDS, School of Management and Engineering Vaud, HES-SO University of Applied Sciences and Arts Western Switzerland, Delémont, Switzerland
| | - Alice Maria Piccirillo
- Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli “Parthenope”, Napoli, Italy
| | - Ferdinand Plaschke
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | - Szymon Polak
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | | | - Herman Proosa
- Tartu Observatory, University of Tartu, Tartu, Estonia
| | | | - Walter Puccio
- Swedish Institute of Space Physics, Uppsala/Kiruna, Sweden
| | - Sylvain Ranvier
- Royal Belgian Institute of Space Aeronomy, Brussels, Belgium
| | - Sean Raymond
- Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS, Nouvelle-Aquitaine, France
| | - Ingo Richter
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
| | - Martin Rieder
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Roberto Rigamonti
- REDS, School of Management and Engineering Vaud, HES-SO University of Applied Sciences and Arts Western Switzerland, Delémont, Switzerland
| | | | - Ondrej Santolik
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | - Takahiro Sasaki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | | | | | | | | | - Jan Soucek
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | | | - Linus Stöckli
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Paweł Szewczyk
- Space Research Centre of the Polish Academy of Sciences, Warsaw, Poland
| | | | - Ludek Uhlir
- Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czech Republic
| | - Naoto Usami
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | - Aris Valavanoglou
- Austrian Academy of Sciences, Space Research Institute, Graz, Austria
| | | | - Wei Wang
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Xiao-Dong Wang
- Swedish Institute of Space Physics, Uppsala/Kiruna, Sweden
| | - Gaëtan Wattieaux
- Laboratoire Plasma et Conversion d’Energie (LAPLACE), CNRS, Université de Toulouse 3, Toulouse, France
| | - Martin Wieser
- Swedish Institute of Space Physics, Uppsala/Kiruna, Sweden
| | - Sebastian Wolf
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Bern, Switzerland
| | - Hajime Yano
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kanagawa, Japan
| | | | - Vladimir Zakharov
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, Paris, France
| | | | - Paola Zuppella
- CNR-Institute for Photonics and Nanotechnologies, Padova, Italy
| | | | - Hantao Ji
- Department of Astrophysical Sciences, Princeton University, Princeton, USA
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3
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Goetz C, Behar E, Beth A, Bodewits D, Bromley S, Burch J, Deca J, Divin A, Eriksson AI, Feldman PD, Galand M, Gunell H, Henri P, Heritier K, Jones GH, Mandt KE, Nilsson H, Noonan JW, Odelstad E, Parker JW, Rubin M, Simon Wedlund C, Stephenson P, Taylor MGGT, Vigren E, Vines SK, Volwerk M. The Plasma Environment of Comet 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2022; 218:65. [PMID: 36397966 PMCID: PMC9649581 DOI: 10.1007/s11214-022-00931-1] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/03/2021] [Accepted: 10/20/2022] [Indexed: 06/04/2023]
Abstract
The environment of a comet is a fascinating and unique laboratory to study plasma processes and the formation of structures such as shocks and discontinuities from electron scales to ion scales and above. The European Space Agency's Rosetta mission collected data for more than two years, from the rendezvous with comet 67P/Churyumov-Gerasimenko in August 2014 until the final touch-down of the spacecraft end of September 2016. This escort phase spanned a large arc of the comet's orbit around the Sun, including its perihelion and corresponding to heliocentric distances between 3.8 AU and 1.24 AU. The length of the active mission together with this span in heliocentric and cometocentric distances make the Rosetta data set unique and much richer than sets obtained with previous cometary probes. Here, we review the results from the Rosetta mission that pertain to the plasma environment. We detail all known sources and losses of the plasma and typical processes within it. The findings from in-situ plasma measurements are complemented by remote observations of emissions from the plasma. Overviews of the methods and instruments used in the study are given as well as a short review of the Rosetta mission. The long duration of the Rosetta mission provides the opportunity to better understand how the importance of these processes changes depending on parameters like the outgassing rate and the solar wind conditions. We discuss how the shape and existence of large scale structures depend on these parameters and how the plasma within different regions of the plasma environment can be characterised. We end with a non-exhaustive list of still open questions, as well as suggestions on how to answer them in the future.
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Affiliation(s)
- Charlotte Goetz
- ESTEC, European Space Agency, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
- Department of Mathematics, Physics and Electrical Engineering, Northumbria University, Newcastle-upon-Tyne, UK
| | - Etienne Behar
- Swedish Institute of Space Physics, Box 812, 981 28 Kiruna, Sweden
- Lagrange, OCA, UCA, CNRS, Nice, France
| | - Arnaud Beth
- Department of Physics, Umeå University, 901 87 Umeå, Sweden
| | - Dennis Bodewits
- Physics Department, Leach Science Center, Auburn University, Auburn, AL 36832 USA
| | - Steve Bromley
- Physics Department, Leach Science Center, Auburn University, Auburn, AL 36832 USA
| | - Jim Burch
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, TX 78228-0510 USA
| | - Jan Deca
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, 3665 Discovery Drive, Boulder, CO 80303 USA
| | - Andrey Divin
- Earth Physics Department, St. Petersburg State University, Ulianovskaya, 1, St Petersburg, 198504 Russia
| | | | - Paul D. Feldman
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 USA
| | - Marina Galand
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ UK
| | - Herbert Gunell
- Department of Physics, Umeå University, 901 87 Umeå, Sweden
| | - Pierre Henri
- Lagrange, OCA, UCA, CNRS, Nice, France
- LPC2E, CNRS, Orléans, France
| | - Kevin Heritier
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ UK
| | - Geraint H. Jones
- UCL Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, RH5 6NT UK
- The Centre for Planetary Sciences at UCL/Birkbeck, Gower Street, London, WC1E 6BT UK
| | | | - Hans Nilsson
- Swedish Institute of Space Physics, Box 812, 981 28 Kiruna, Sweden
| | - John W. Noonan
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85719 USA
| | - Elias Odelstad
- Swedish Institute of Space Physics, Box 537, SE-751 21 Uppsala, Sweden
| | | | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Cyril Simon Wedlund
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria
| | - Peter Stephenson
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ UK
| | | | - Erik Vigren
- Swedish Institute of Space Physics, Box 537, SE-751 21 Uppsala, Sweden
| | - Sarah K. Vines
- Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723 USA
| | - Martin Volwerk
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 8042 Graz, Austria
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4
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Zhang S, Wu Y, Zhang Z, Luo Z, Zhao Y, Li Z, Chang Y, Yang J, Wu G, Zhang W, Yu S, Yuan K, Yang X. Photodissociation dynamics of CO2 + hv → CO(X1Σ+) + O(1D2) via the 3P1Πu state. J Chem Phys 2022; 156:054302. [DOI: 10.1063/5.0081489] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Affiliation(s)
- Su’e Zhang
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang Province, People’s Republic of China
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Yucheng Wu
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang Province, People’s Republic of China
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Zhaoxue Zhang
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang Province, People’s Republic of China
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Zijie Luo
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Yarui Zhao
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Zhenxing Li
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Yao Chang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Jiayue Yang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Guorong Wu
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Weiqing Zhang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Shengrui Yu
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou 311231, Zhejiang Province, People’s Republic of China
| | - Kaijun Yuan
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
| | - Xueming Yang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, 457 Zhongshan Road, Dalian 116023, Liaoning Province, People’s Republic of China
- Department of Chemistry, College of Science, Southern University of Science and Technology, Shenzhen 518055, People’s Republic of China
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5
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Three body photodissociation of the water molecule and its implications for prebiotic oxygen production. Nat Commun 2021; 12:2476. [PMID: 33931653 PMCID: PMC8087761 DOI: 10.1038/s41467-021-22824-7] [Citation(s) in RCA: 6] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/14/2020] [Accepted: 04/01/2021] [Indexed: 11/20/2022] Open
Abstract
The provenance of oxygen on the Earth and other planets in the Solar System is a fundamental issue. It has been widely accepted that the only prebiotic pathway to produce oxygen in the Earth’s primitive atmosphere was via vacuum ultraviolet (VUV) photodissociation of CO2 and subsequent two O atom recombination. Here, we provide experimental evidence of three-body dissociation (TBD) of H2O to produce O atoms in both 1D and 3P states upon VUV excitation using a tunable VUV free electron laser. Experimental results show that the TBD is the dominant pathway in the VUV H2O photochemistry at wavelengths between 90 and 107.4 nm. The relative abundance of water in the interstellar space with its exposure to the intense VUV radiation suggests that the TBD of H2O and subsequent O atom recombination should be an important prebiotic O2-production, which may need to be incorporated into interstellar photochemical models. Three-body dissociation of water, producing one oxygen and two hydrogen atoms, has been difficult to investigate due to the lack of intense vacuum ultraviolet sources. Here, using a tunable free-electron laser, the authors obtain quantum yields for this channel showing that it is a possible route to prebiotic oxygen formation in interstellar environments.
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6
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Marschall R, Skorov Y, Zakharov V, Rezac L, Gerig SB, Christou C, Dadzie SK, Migliorini A, Rinaldi G, Agarwal J, Vincent JB, Kappel D. Cometary Comae-Surface Links: The Physics of Gas and Dust from the Surface to a Spacecraft. SPACE SCIENCE REVIEWS 2020; 216:130. [PMID: 33184519 PMCID: PMC7647976 DOI: 10.1007/s11214-020-00744-0] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/28/2019] [Accepted: 09/28/2020] [Indexed: 06/04/2023]
Abstract
A comet is a highly dynamic object, undergoing a permanent state of change. These changes have to be carefully classified and considered according to their intrinsic temporal and spatial scales. The Rosetta mission has, through its contiguous in-situ and remote sensing coverage of comet 67P/Churyumov-Gerasimenko (hereafter 67P) over the time span of August 2014 to September 2016, monitored the emergence, culmination, and winding down of the gas and dust comae. This provided an unprecedented data set and has spurred a large effort to connect in-situ and remote sensing measurements to the surface. In this review, we address our current understanding of cometary activity and the challenges involved when linking comae data to the surface. We give the current state of research by describing what we know about the physical processes involved from the surface to a few tens of kilometres above it with respect to the gas and dust emission from cometary nuclei. Further, we describe how complex multidimensional cometary gas and dust models have developed from the Halley encounter of 1986 to today. This includes the study of inhomogeneous outgassing and determination of the gas and dust production rates. Additionally, the different approaches used and results obtained to link coma data to the surface will be discussed. We discuss forward and inversion models and we describe the limitations of the respective approaches. The current literature suggests that there does not seem to be a single uniform process behind cometary activity. Rather, activity seems to be the consequence of a variety of erosion processes, including the sublimation of both water ice and more volatile material, but possibly also more exotic processes such as fracture and cliff erosion under thermal and mechanical stress, sub-surface heat storage, and a complex interplay of these processes. Seasons and the nucleus shape are key factors for the distribution and temporal evolution of activity and imply that the heliocentric evolution of activity can be highly individual for every comet, and generalisations can be misleading.
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Affiliation(s)
- Raphael Marschall
- Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO 80302 USA
- International Space Science Institute (ISSI), Hallerstrasse 6, 3012 Bern, Switzerland
| | - Yuri Skorov
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | | | - Ladislav Rezac
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Selina-Barbara Gerig
- Physikalisches Institut, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland
- NCCR PlanetS, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Chariton Christou
- School of Engineering and Physical Sciences, Heriot-Watt University, Edinburgh, EH14 4AS Scotland UK
| | - S. Kokou Dadzie
- School of Engineering and Physical Sciences, Heriot-Watt University, Edinburgh, EH14 4AS Scotland UK
| | | | | | - Jessica Agarwal
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Jean-Baptiste Vincent
- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Planetenforschung, Rutherfordstrasse 2, 12489 Berlin, Germany
| | - David Kappel
- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Planetenforschung, Rutherfordstrasse 2, 12489 Berlin, Germany
- Institute of Physics and Astronomy, University of Potsdam, Potsdam-Golm, Germany
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7
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Piani L, Marrocchi Y, Rigaudier T, Vacher LG, Thomassin D, Marty B. Earth’s water may have been inherited from material similar to enstatite chondrite meteorites. Science 2020; 369:1110-1113. [DOI: 10.1126/science.aba1948] [Citation(s) in RCA: 98] [Impact Index Per Article: 24.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/22/2019] [Accepted: 07/15/2020] [Indexed: 11/02/2022]
Abstract
The origin of Earth’s water remains unknown. Enstatite chondrite (EC) meteorites have similar isotopic composition to terrestrial rocks and thus may be representative of the material that formed Earth. ECs are presumed to be devoid of water because they formed in the inner Solar System. Earth’s water is therefore generally attributed to the late addition of a small fraction of hydrated materials, such as carbonaceous chondrite meteorites, which originated in the outer Solar System where water was more abundant. We show that EC meteorites contain sufficient hydrogen to have delivered to Earth at least three times the mass of water in its oceans. EC hydrogen and nitrogen isotopic compositions match those of Earth’s mantle, so EC-like asteroids might have contributed these volatile elements to Earth’s crust and mantle.
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Affiliation(s)
- Laurette Piani
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Centre National de Recherche Scientifique (CNRS)–Université de Lorraine, Vandoeuvre-les-Nancy, F-54500, France
| | - Yves Marrocchi
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Centre National de Recherche Scientifique (CNRS)–Université de Lorraine, Vandoeuvre-les-Nancy, F-54500, France
| | - Thomas Rigaudier
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Centre National de Recherche Scientifique (CNRS)–Université de Lorraine, Vandoeuvre-les-Nancy, F-54500, France
| | - Lionel G. Vacher
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Centre National de Recherche Scientifique (CNRS)–Université de Lorraine, Vandoeuvre-les-Nancy, F-54500, France
- Department of Physics, Washington University in St. Louis, St. Louis, MO 63130, USA
| | - Dorian Thomassin
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Centre National de Recherche Scientifique (CNRS)–Université de Lorraine, Vandoeuvre-les-Nancy, F-54500, France
| | - Bernard Marty
- Centre de Recherches Pétrographiques et Géochimiques (CRPG), Centre National de Recherche Scientifique (CNRS)–Université de Lorraine, Vandoeuvre-les-Nancy, F-54500, France
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8
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Rubin M, Engrand C, Snodgrass C, Weissman P, Altwegg K, Busemann H, Morbidelli A, Mumma M. On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2020; 216:102. [PMID: 32801398 PMCID: PMC7392949 DOI: 10.1007/s11214-020-00718-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/09/2019] [Accepted: 07/03/2020] [Indexed: 06/02/2023]
Abstract
Primitive objects like comets hold important information on the material that formed our solar system. Several comets have been visited by spacecraft and many more have been observed through Earth- and space-based telescopes. Still our understanding remains limited. Molecular abundances in comets have been shown to be similar to interstellar ices and thus indicate that common processes and conditions were involved in their formation. The samples returned by the Stardust mission to comet Wild 2 showed that the bulk refractory material was processed by high temperatures in the vicinity of the early sun. The recent Rosetta mission acquired a wealth of new data on the composition of comet 67P/Churyumov-Gerasimenko (hereafter 67P/C-G) and complemented earlier observations of other comets. The isotopic, elemental, and molecular abundances of the volatile, semi-volatile, and refractory phases brought many new insights into the origin and processing of the incorporated material. The emerging picture after Rosetta is that at least part of the volatile material was formed before the solar system and that cometary nuclei agglomerated over a wide range of heliocentric distances, different from where they are found today. Deviations from bulk solar system abundances indicate that the material was not fully homogenized at the location of comet formation, despite the radial mixing implied by the Stardust results. Post-formation evolution of the material might play an important role, which further complicates the picture. This paper discusses these major findings of the Rosetta mission with respect to the origin of the material and puts them in the context of what we know from other comets and solar system objects.
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Affiliation(s)
- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Cécile Engrand
- CNRS/IN2P3, IJCLab, Université Paris-Saclay, 91405 Orsay Cedex, France
| | - Colin Snodgrass
- Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ UK
| | | | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Henner Busemann
- Institute of Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | | | - Michael Mumma
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, 20771 MD USA
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9
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Zhou J, Luo Z, Yang J, Chang Y, Zhang Z, Yu Y, Li Q, Cheng G, Chen Z, He Z, Che L, Yu S, Wu G, Yuan K, Yang X. State-to-state photodissociation dynamics of CO 2 around 108 nm: the O( 1S) atom channel. Phys Chem Chem Phys 2020; 22:6260-6265. [PMID: 32129384 DOI: 10.1039/c9cp06919d] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
State-to-state photodissociation of carbon dioxide (CO2) via the 3p1Πu Rydberg state was investigated by the time-sliced velocity map ion imaging technique (TSVMI) using a tunable vacuum ultraviolet free electron laser (VUV FEL) source. Raw images of the O(1S) products resulting from the O(1S) + CO(X1Σ+) channel were acquired at the photolysis wavelengths between 107.37 and 108.84 nm. From the vibrational resolved O(1S) images, the product total kinetic energy releases and the vibrational state distributions of the CO(X1Σ+) co-products were obtained, respectively. It is found that vibrationally excited CO co-products populate at as high as v = 6 or 7 while peaking at v = 1 and v = 4, and most of the individual vibrational peaks present a bimodal rotational structure. Furthermore, the angular distributions at all studied photolysis wavelengths have also been determined. The associated vibrational-state specific anisotropy parameters (β) exhibit a photolysis wavelength-dependent feature, in which the β-values observed at 108.01 nm and 108.27 nm are more positive than those at 107.37 nm and 107.52 nm, while the β-values have almost isotropic behaviour at 108.84 nm. These experimental results indicate that the initially prepared CO2 molecules around 108 nm should decay to the 41A' state via non-adiabatic coupling, and dissociate in the 41A' state to produce O(1S) + CO(X1Σ+) products with different dissociation time scales.
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Affiliation(s)
- Jiami Zhou
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou, Zhejiang 311231, China. and State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Zijie Luo
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China. and Department of Physics, School of Science, Dalian Maritime University, 1 Linghai Road, Dalian, Liaoning 116026, P. R. China
| | - Jiayue Yang
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Yao Chang
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Zhiguo Zhang
- Key Laboratory of Functional Materials and Devices for Informatics of Anhui Higher Education Institutions and School of Physics and Electronic Engineering, Fuyang Normal University, Fuyang, Anhui 236041, China.
| | - Yong Yu
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Qinming Li
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Gongkui Cheng
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Zhichao Chen
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Zhigang He
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Li Che
- Department of Physics, School of Science, Dalian Maritime University, 1 Linghai Road, Dalian, Liaoning 116026, P. R. China
| | - Shengrui Yu
- Hangzhou Institute of Advanced Studies, Zhejiang Normal University, 1108 Gengwen Road, Hangzhou, Zhejiang 311231, China.
| | - Guorong Wu
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Kaijun Yuan
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
| | - Xueming Yang
- State Key Laboratory of Molecular Reaction Dynamics, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian, Liaoning 116023, China.
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10
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Rubin M, Engrand C, Snodgrass C, Weissman P, Altwegg K, Busemann H, Morbidelli A, Mumma M. On the Origin and Evolution of the Material in 67P/Churyumov-Gerasimenko. SPACE SCIENCE REVIEWS 2020. [PMID: 32801398 DOI: 10.1007/s11214-019-0625-7] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
Primitive objects like comets hold important information on the material that formed our solar system. Several comets have been visited by spacecraft and many more have been observed through Earth- and space-based telescopes. Still our understanding remains limited. Molecular abundances in comets have been shown to be similar to interstellar ices and thus indicate that common processes and conditions were involved in their formation. The samples returned by the Stardust mission to comet Wild 2 showed that the bulk refractory material was processed by high temperatures in the vicinity of the early sun. The recent Rosetta mission acquired a wealth of new data on the composition of comet 67P/Churyumov-Gerasimenko (hereafter 67P/C-G) and complemented earlier observations of other comets. The isotopic, elemental, and molecular abundances of the volatile, semi-volatile, and refractory phases brought many new insights into the origin and processing of the incorporated material. The emerging picture after Rosetta is that at least part of the volatile material was formed before the solar system and that cometary nuclei agglomerated over a wide range of heliocentric distances, different from where they are found today. Deviations from bulk solar system abundances indicate that the material was not fully homogenized at the location of comet formation, despite the radial mixing implied by the Stardust results. Post-formation evolution of the material might play an important role, which further complicates the picture. This paper discusses these major findings of the Rosetta mission with respect to the origin of the material and puts them in the context of what we know from other comets and solar system objects.
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Affiliation(s)
- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Cécile Engrand
- CNRS/IN2P3, IJCLab, Université Paris-Saclay, 91405 Orsay Cedex, France
| | - Colin Snodgrass
- Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ UK
| | | | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
| | - Henner Busemann
- Institute of Geochemistry and Petrology, Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | | | - Michael Mumma
- NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, 20771 MD USA
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11
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Combi M, Shou Y, Fougere N, Tenishev V, Altwegg K, Rubin M, Bockelée-Morvan D, Capaccioni F, Cheng YC, Fink U, Gombosi T, Hansen KC, Huang Z, Marshall D, Toth G. The Surface Distributions of the Production of the Major Volatile Species, H 2O, CO 2, CO and O 2, from the Nucleus of Comet 67P/Churyumov-Gerasimenko throughout the Rosetta Mission as Measured by the ROSINA Double Focusing Mass Spectrometer. ICARUS 2020; 335:113421. [PMID: 31631900 PMCID: PMC6800715 DOI: 10.1016/j.icarus.2019.113421] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) suite of instruments operated throughout the over two years of the Rosetta mission operations in the vicinity of comet 67P/Churyumov-Gerasimenko. It measured gas densities and composition throughout the comet's atmosphere, or coma. Here we present two-years' worth of measurements of the relative densities of the four major volatile species in the coma of the comet, H2O, CO2, CO and O2, by one of the ROSINA sub-systems called the Double Focusing Mass Spectrometer (DFMS). The absolute total gas densities were provided by the Comet Pressure Sensor (COPS), another ROSINA sub-system. DFMS is a very high mass resolution and high sensitivity mass spectrometer able to resolve at a tiny fraction of an atomic mass unit. We have analyzed the combined DFMS and COPS measurements using an inversion scheme based on spherical harmonics that solves for the distribution of potential surface activity of each species as the comet rotates, changing solar illumination, over short time intervals and as the comet changes distance from the sun and orientation of its spin axis over long time intervals. We also use the surface boundary conditions derived from the inversion scheme to simulate the whole coma with our fully kinetic Direct Simulation Monte Carlo model and calculate the production rates of the four major species throughout the mission. We compare the derived production rates with revised remote sensing observations by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) as well as with published observations from the Microwave Instrument for the Rosetta Orbiter (MIRO). Finally we use the variation of the surface production of the major species to calculate the total mass loss over the mission and, for different estimates of the dust/gas ratio, calculate the variation of surface loss all over the nucleus.
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Affiliation(s)
- Michael Combi
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - Yinsi Shou
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - Nicolas Fougere
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - Valeriy Tenishev
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Bern, Switzerland
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Bern, Switzerland
| | - Dominique Bockelée-Morvan
- LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites, UPMC Univ. Paris 06, Univ. Paris-Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, F-92195 Meudon, France
| | - Fabrizio Capaccioni
- 4INAF-IAPS, Istituto di Astrofisica e Planetologia Spaziali, via del fosso del Cavaliere 100, I-00133 Rome, Italy
| | - Yu-Chi Cheng
- LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites, UPMC Univ. Paris 06, Univ. Paris-Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, F-92195 Meudon, France
| | - Uwe Fink
- Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA
| | - Tamas Gombosi
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - Kenneth C Hansen
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - Zhenguang Huang
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - David Marshall
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Gabor Toth
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
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Luspay-Kuti A, Altwegg K, Berthelier JJ, Beth A, Dhooghe F, Fiethe B, Fuselier SA, Gombosi TI, Hansen KC, Hässig M, Livadiotis G, Mall U, Mandt KE, Mousis O, Petrinec SM, Rubin M, Trattner KJ, Tzou CY, Wurz P. Comparison of neutral outgassing of comet 67P/Churyumov-Gerasimenko inbound and outbound beyond 3 AU from ROSINA/DFMS. ASTRONOMY AND ASTROPHYSICS 2019; 630:A30. [PMID: 32699429 PMCID: PMC7375265 DOI: 10.1051/0004-6361/201833536] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
CONTEXT Pre-equinox measurements of comet 67P/Churyumov-Gerasimenko with the mass spectrometer ROSINA/DFMS on board the Rosetta spacecraft revealed a strongly heterogeneous coma. The abundances of major and various minor volatile species were found to depend on the latitude and longitude of the nadir point of the spacecraft. The observed time variability of coma species remained consistent for about three months up to equinox. The chemical variability could be generally interpreted in terms of surface temperature and seasonal effects superposed on some kind of chemical heterogeneity of the nucleus. AIMS We compare here pre-equinox (inbound) ROSINA/DFMS measurements from 2014 to measurements taken after the outbound equinox in 2016, both at heliocentric distances larger than 3 AU. For a direct comparison we limit our observations to the southern hemisphere. METHODS We report the similarities and differences in the concentrations and time variability of neutral species under similar insolation conditions (heliocentric distance and season) pre- and post-equinox, and interpret them in light of the previously published observations. In addition, we extend both the pre- and post-equinox analysis by comparing species concentrations with a mixture of CO2 and H2O. RESULTS Our results show significant changes in the abundances of neutral species in the coma from pre- to post-equinox that are indicative of seasonally driven nucleus heterogeneity. CONCLUSIONS The observed pre- and post-equinox patterns can generally be explained by the strong erosion in the southern hemisphere that moves volatile-rich layers near the surface.
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Affiliation(s)
- A Luspay-Kuti
- Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA
| | - K Altwegg
- Physikalisches Institut, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland
- Center for Space and Habitability (CSH), Universität Bern, Sidlerstr. 5, 3012 Bern, Switzerland
| | - J J Berthelier
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Institut Pierre Simon Laplace, CNRS, Université Pierre et Marie Curie, 4 avenue de Neptune, 94100 Saint-Maur, France
| | - A Beth
- Department of Physics/SPAT, Imperial College London, London SW7 2AZ, UK
| | - F Dhooghe
- Belgian Institute for Space Aeronomy, BIRA-IASB, Ringlaan 3, 1180 Brussels, Belgium
- Center for Plasma Astrophysics, K.U. Leuven, Celestijnenlaan 200D, 3001 Heverlee, Belgium
| | - B Fiethe
- Institute of Computer and Network Engineering (IDA), TU Braunschweig, Hans-Sommer-Strasse 66, 38106 Braunschweig, Germany
| | - S A Fuselier
- Space Science Directorate, Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX 78228, USA
| | - T I Gombosi
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - K C Hansen
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - M Hässig
- Space Science Directorate, Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX 78228, USA
| | - G Livadiotis
- Space Science Directorate, Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX 78228, USA
| | - U Mall
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - K E Mandt
- Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA
| | - O Mousis
- Laboratoire d'Astrophysique de Marseille, CNRS, Aix Marseille Université, 13388 Marseille, France
| | - S M Petrinec
- Lockheed Martin Space Systems Advanced Technology Center, 3251 Hanover St., Palo Alto, CA 94304, USA
| | - M Rubin
- Physikalisches Institut, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland
| | - K J Trattner
- Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, 3665 Discovery Dr., Boulder, CO 80309, USA
| | - C-Y Tzou
- Physikalisches Institut, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland
| | - P Wurz
- Physikalisches Institut, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland
- Center for Space and Habitability (CSH), Universität Bern, Sidlerstr. 5, 3012 Bern, Switzerland
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Noble Gas Abundance Ratios Indicate the Agglomeration of 67P/Churyumov–Gerasimenko from Warmed-up Ice. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aadf89] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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14
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Rubin M, Altwegg K, Balsiger H, Bar-Nun A, Berthelier JJ, Briois C, Calmonte U, Combi M, De Keyser J, Fiethe B, Fuselier SA, Gasc S, Gombosi TI, Hansen KC, Kopp E, Korth A, Laufer D, Le Roy L, Mall U, Marty B, Mousis O, Owen T, Rème H, Sémon T, Tzou CY, Waite JH, Wurz P. Krypton isotopes and noble gas abundances in the coma of comet 67P/Churyumov-Gerasimenko. SCIENCE ADVANCES 2018; 4:eaar6297. [PMID: 29978041 PMCID: PMC6031375 DOI: 10.1126/sciadv.aar6297] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/06/2017] [Accepted: 05/24/2018] [Indexed: 05/15/2023]
Abstract
The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis mass spectrometer Double Focusing Mass Spectrometer on board the European Space Agency's Rosetta spacecraft detected the major isotopes of the noble gases argon, krypton, and xenon in the coma of comet 67P/Churyumov-Gerasimenko. Earlier, it was found that xenon exhibits an isotopic composition distinct from anywhere else in the solar system. However, argon isotopes, within error, were shown to be consistent with solar isotope abundances. This discrepancy suggested an additional exotic component of xenon in comet 67P/Churyumov-Gerasimenko. We show that krypton also exhibits an isotopic composition close to solar. Furthermore, we found the argon to krypton and the krypton to xenon ratios in the comet to be lower than solar, which is a necessity to postulate an addition of exotic xenon in the comet.
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Affiliation(s)
- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Corresponding author.
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, CH-3012 Bern, Switzerland
| | - Hans Balsiger
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Akiva Bar-Nun
- Department of Geophysics, Tel Aviv University, Ramat-Aviv, Tel Aviv, Israel
| | - Jean-Jacques Berthelier
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Institut Pierre Simon Laplace, CNRS, Université Pierre et Marie Curie, 4 Place Jussieu, 75252 Paris Cedex 05, France
| | - Christelle Briois
- Laboratoire de Physique et Chimie de l’Environnement et de l’Espace, UMR 6115 CNRS–Université d’Orléans, Orléans, France
| | - Ursina Calmonte
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Michael Combi
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Johan De Keyser
- Koninklijk Belgisch Instituut voor Ruimte-Aeronomie–Institut Royal Belge d’Aéronomie Spatiale, Ringlaan 3, B-1180 Brussels, Belgium
| | - Björn Fiethe
- Institute of Computer and Network Engineering, Technische Universität Braunschweig, Hans-Sommer-Straße 66, D-38106 Braunschweig, Germany
| | - Stephen A. Fuselier
- Space Science Directorate, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
- University of Texas at San Antonio, San Antonio, TX 78249, USA
| | - Sebastien Gasc
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Tamas I. Gombosi
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Kenneth C. Hansen
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Ernest Kopp
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Axel Korth
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Diana Laufer
- Department of Geophysics, Tel Aviv University, Ramat-Aviv, Tel Aviv, Israel
| | - Léna Le Roy
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Urs Mall
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Bernard Marty
- Centre de Recherches Pétrographiques et Géochimiques, CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre lès Nancy, France
| | - Olivier Mousis
- Laboratoire d’Astrophysique de Marseille, CNRS, Aix-Marseille Université, 13388 Marseille, France
| | - Tobias Owen
- Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
| | - Henri Rème
- Institut de Recherche en Astrophysique et Planétologie, CNRS, Université Paul Sabatier, Observatoire Midi-Pyrénées, 9 Avenue du Colonel Roche, 31028 Toulouse Cedex 4, France
- Centre National d’Études Spatiales, 2 Place Maurice Quentin, 75001 Paris, France
| | - Thierry Sémon
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Chia-Yu Tzou
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Jack H. Waite
- Institute of Computer and Network Engineering, Technische Universität Braunschweig, Hans-Sommer-Straße 66, D-38106 Braunschweig, Germany
| | - Peter Wurz
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, CH-3012 Bern, Switzerland
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O'D Alexander CM, McKeegan KD, Altwegg K. Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets. SPACE SCIENCE REVIEWS 2018; 214:36. [PMID: 30842688 PMCID: PMC6398961 DOI: 10.1007/s11214-018-0474-9] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/10/2018] [Accepted: 01/11/2018] [Indexed: 06/09/2023]
Abstract
Asteroids and comets are the remnants of the swarm of planetesimals from which the planets ultimately formed, and they retain records of processes that operated prior to and during planet formation. They are also likely the sources of most of the water and other volatiles accreted by Earth. In this review, we discuss the nature and probable origins of asteroids and comets based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids. The asteroidal parent bodies of meteorites formed ≤4 Ma after Solar System formation while there was still a gas disk present. It seems increasingly likely that the parent bodies of meteorites spectroscopically linked with the E-, S-, M- and V-type asteroids formed sunward of Jupiter's orbit, while those associated with C- and, possibly, D-type asteroids formed further out, beyond Jupiter but probably not beyond Saturn's orbit. Comets formed further from the Sun than any of the meteorite parent bodies, and retain much higher abundances of interstellar material. CI and CM group meteorites are probably related to the most common C-type asteroids, and based on isotopic evidence they, rather than comets, are the most likely sources of the H and N accreted by the terrestrial planets. However, comets may have been major sources of the noble gases accreted by Earth and Venus. Possible constraints that these observations can place on models of giant planet formation and migration are explored.
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Affiliation(s)
- Conel M O'D Alexander
- Dept. Terrestrial Magnetism, Carnegie Institution for Science, 5241 Broad Branch Road NW, Washington, DC 20015, USA. . Tel. (202) 478 8478
| | - Kevin D McKeegan
- Department of Earth, Planetary, and Space Sciences, University of California-Los Angeles, Los Angeles, CA 90095-1567, USA.
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland.
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16
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Turner AM, Abplanalp MJ, Blair TJ, Dayuha R, Kaiser RI. An Infrared Spectroscopic Study Toward the Formation of Alkylphosphonic Acids and Their Precursors in Extraterrestrial Environments. THE ASTROPHYSICAL JOURNAL. SUPPLEMENT SERIES 2018; 234:6. [PMID: 30842689 PMCID: PMC6398957 DOI: 10.3847/1538-4365/aa9183] [Citation(s) in RCA: 15] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
The only known phosphorus-containing organic compounds of extraterrestrial origin, alkylphosphonic acids, were discovered in the Murchison meteorite and have accelerated the hypothesis that reduced oxidation states of phosphorus were delivered to early Earth and served as a prebiotic source of phosphorus. While previous studies looking into the formation of these alkylphosphonic acids have focused on the iron-nickel phosphide mineral schreibersite and phosphorous acid as a source of phosphorus, this work utilizes phosphine (PH3), which has been discovered in the circumstellar envelope of IRC +10216, in the atmosphere of Jupiter and Saturn, and believed to be the phosphorus carrier in comet 67P/Churyumov-Gerasimenko. Phosphine ices prepared with interstellar molecules such as carbon dioxide, water, and methane were subjected to electron irradiation, which simulates the secondary electrons produced from galactic cosmic rays penetrating the ice, and probed using infrared spectroscopy to understand the possible formation of alkylphosphonic acids and their precursors on interstellar icy grains that could become incorporated into meteorites such as Murchison. We present the first study and results on the possible synthesis of alkylphosphonic acids produced from phosphine-mixed ices under interstellar conditions. All functional groups of alkylphosphonic acids were detected through infrared spectroscopically, suggesting that this class of molecules can be formed in interstellar ices.
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Affiliation(s)
- Andrew M Turner
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA;
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA
| | - Matthew J Abplanalp
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA;
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA
| | - Tyler J Blair
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA;
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA
| | - Remwilyn Dayuha
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA;
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA
| | - Ralf I Kaiser
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA;
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, USA
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17
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Snodgrass C, A'Hearn MF, Aceituno F, Afanasiev V, Bagnulo S, Bauer J, Bergond G, Besse S, Biver N, Bodewits D, Boehnhardt H, Bonev BP, Borisov G, Carry B, Casanova V, Cochran A, Conn BC, Davidsson B, Davies JK, de León J, de Mooij E, de Val-Borro M, Delacruz M, DiSanti MA, Drew JE, Duffard R, Edberg NJT, Faggi S, Feaga L, Fitzsimmons A, Fujiwara H, Gibb EL, Gillon M, Green SF, Guijarro A, Guilbert-Lepoutre A, Gutiérrez PJ, Hadamcik E, Hainaut O, Haque S, Hedrosa R, Hines D, Hopp U, Hoyo F, Hutsemékers D, Hyland M, Ivanova O, Jehin E, Jones GH, Keane JV, Kelley MSP, Kiselev N, Kleyna J, Kluge M, Knight MM, Kokotanekova R, Koschny D, Kramer EA, López-Moreno JJ, Lacerda P, Lara LM, Lasue J, Lehto HJ, Levasseur-Regourd AC, Licandro J, Lin ZY, Lister T, Lowry SC, Mainzer A, Manfroid J, Marchant J, McKay AJ, McNeill A, Meech KJ, Micheli M, Mohammed I, Monguió M, Moreno F, Muñoz O, Mumma MJ, Nikolov P, Opitom C, Ortiz JL, Paganini L, Pajuelo M, Pozuelos FJ, Protopapa S, Pursimo T, Rajkumar B, Ramanjooloo Y, Ramos E, Ries C, Riffeser A, Rosenbush V, Rousselot P, Ryan EL, Santos-Sanz P, Schleicher DG, Schmidt M, Schulz R, Sen AK, Somero A, Sota A, Stinson A, Sunshine JM, Thompson A, Tozzi GP, Tubiana C, Villanueva GL, Wang X, Wooden DH, Yagi M, Yang B, Zaprudin B, Zegmott TJ. The 67P/Churyumov-Gerasimenko observation campaign in support of the Rosetta mission. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2016.0249. [PMID: 28554971 PMCID: PMC5454223 DOI: 10.1098/rsta.2016.0249] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 11/21/2016] [Indexed: 05/15/2023]
Abstract
We present a summary of the campaign of remote observations that supported the European Space Agency's Rosetta mission. Telescopes across the globe (and in space) followed comet 67P/Churyumov-Gerasimenko from before Rosetta's arrival until nearly the end of the mission in September 2016. These provided essential data for mission planning, large-scale context information for the coma and tails beyond the spacecraft and a way to directly compare 67P with other comets. The observations revealed 67P to be a relatively 'well-behaved' comet, typical of Jupiter family comets and with activity patterns that repeat from orbit to orbit. Comparison between this large collection of telescopic observations and the in situ results from Rosetta will allow us to better understand comet coma chemistry and structure. This work is just beginning as the mission ends-in this paper, we present a summary of the ground-based observations and early results, and point to many questions that will be addressed in future studies.This article is part of the themed issue 'Cometary science after Rosetta'.
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Affiliation(s)
- C Snodgrass
- School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
| | - M F A'Hearn
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - F Aceituno
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - V Afanasiev
- Special Astrophysical Observatory, Russian Academy of Sciences, Nizhny Arkhyz, Russia
| | - S Bagnulo
- Armagh Observatory, College Hill, Armagh BT61 9DG, UK
| | - J Bauer
- Jet Propulsion Laboratory, M/S 183-401, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - G Bergond
- Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal (Almería), Spain
| | - S Besse
- ESA/ESAC, PO Box 78, 28691 Villanueva de la Cañada, Spain
| | - N Biver
- LESIA, Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France
| | - D Bodewits
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - H Boehnhardt
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - B P Bonev
- Department of Physics, American University, 4400 Massachusetts Avenue NW, Washington, DC 20016, USA
| | - G Borisov
- Armagh Observatory, College Hill, Armagh BT61 9DG, UK
- Institute of Astronomy and National Astronomical Observatory, 72 Tsarigradsko Chaussée Boulevard, BG-1784 Sofia, Bulgaria
| | - B Carry
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Lagrange, France
- IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Lille, France
| | - V Casanova
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - A Cochran
- University of Texas Austin/McDonald Observatory, 1 University Station, Austin, TX 78712, USA
| | - B C Conn
- Research School of Astronomy and Astrophysics, The Australian National University, Canberra, Australian Capital Territory, Australia
- Gemini Observatory, Recinto AURA, Colina El Pino s/n, Casilla 603, La Serena, Chile
| | - B Davidsson
- Jet Propulsion Laboratory, M/S 183-401, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - J K Davies
- The UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - J de León
- Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain
- Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
| | - E de Mooij
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
| | - M de Val-Borro
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
- NASA Goddard Space Flight Center, Astrochemistry Laboratory, Code 693.0, Greenbelt, MD 20771, USA
- Department of Physics, The Catholic University of America, Washington, DC 20064, USA
| | - M Delacruz
- Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - M A DiSanti
- NASA Goddard Space Flight Center, Astrochemistry Laboratory, Code 693.0, Greenbelt, MD 20771, USA
| | - J E Drew
- School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
| | - R Duffard
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - N J T Edberg
- Swedish Institute of Space Physics, Ångströmlaboratoriet, Lägerhyddsvägen 1, 751 21 Uppsala, Sweden
| | - S Faggi
- INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50 125 Firenze, Italy
| | - L Feaga
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - A Fitzsimmons
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
| | - H Fujiwara
- Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720, USA
| | - E L Gibb
- Department of Physics and Astronomy, University of Missouri - St. Louis, St. Louis, MO 63121, USA
| | - M Gillon
- Institut d'Astrophysique et de Géophysique, Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
| | - S F Green
- School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
| | - A Guijarro
- Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal (Almería), Spain
| | - A Guilbert-Lepoutre
- Institut UTINAM, UMR 6213 CNRS-Université de Franche Comté, Besançon, France
| | - P J Gutiérrez
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - E Hadamcik
- CNRS/INSU; UPMC (Sorbonne Univ.); UVSQ (UPSay); LATMOS-IPSL, 11 Bld d'Alembert, 78280 Guyancourt, France
| | - O Hainaut
- European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
| | - S Haque
- Department of Physics, University of the West Indies, St Augustine, Trinidad, West Indies
| | - R Hedrosa
- Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal (Almería), Spain
| | - D Hines
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - U Hopp
- University Observatory, Ludwig-Maximilian-University Munich, Scheiner Strasse 1, 81679 Munich, Germany
| | - F Hoyo
- Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal (Almería), Spain
| | - D Hutsemékers
- Institut d'Astrophysique et de Géophysique, Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
| | - M Hyland
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
| | - O Ivanova
- Astronomical Institute of the Slovak Academy of Sciences, 05960 Tatranská Lomnica, Slovak Republic
| | - E Jehin
- Institut d'Astrophysique et de Géophysique, Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
| | - G H Jones
- Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT, UK
- The Centre for Planetary Sciences at UCL/Birkbeck, Gower Street, London WC1E 6BT, UK
| | - J V Keane
- Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - M S P Kelley
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - N Kiselev
- Main Astronomical Observatory of National Academy of Sciences, Kyiv, UKraine
| | - J Kleyna
- Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - M Kluge
- University Observatory, Ludwig-Maximilian-University Munich, Scheiner Strasse 1, 81679 Munich, Germany
| | - M M Knight
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - R Kokotanekova
- School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - D Koschny
- Research and Scientific Support Department, European Space Agency, 2201 Noordwijk, The Netherlands
| | - E A Kramer
- Jet Propulsion Laboratory, M/S 183-401, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - J J López-Moreno
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - P Lacerda
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
| | - L M Lara
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - J Lasue
- Université de Toulouse, UPS-OMP, IRAP-CNRS, Toulouse, France
| | - H J Lehto
- Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
| | - A C Levasseur-Regourd
- UPMC (Sorbonne Univ.); UVSQ (UPSay); CNRS/INSU; LATMOS-IPSL, BC 102, 4 Place Jussieu, 75005 Paris, France
| | - J Licandro
- Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain
- Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
| | - Z Y Lin
- Graduate Institute of Astronomy, National Central University, No. 300 Zhongda Road, Zhongli District, Taoyuan City, 320 Taiwan
| | - T Lister
- Las Cumbres Observatory, 6740 Cortona Drive, Ste. 102, Goleta, CA 93117, USA
| | - S C Lowry
- Centre for Astrophysics and Planetary Science, School of Physical Sciences, The University of Kent, Canterbury CT2 7NH, UK
| | - A Mainzer
- Jet Propulsion Laboratory, M/S 183-401, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - J Manfroid
- Institut d'Astrophysique et de Géophysique, Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
| | - J Marchant
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool L3 5RF, UK
| | - A J McKay
- University of Texas Austin/McDonald Observatory, 1 University Station, Austin, TX 78712, USA
- NASA Goddard Space Flight Center, Astrochemistry Laboratory, Code 693.0, Greenbelt, MD 20771, USA
| | - A McNeill
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
| | - K J Meech
- Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - M Micheli
- ESA SSA-NEO Coordination Centre, Frascati (RM), Italy
| | - I Mohammed
- Caribbean Institute of Astronomy, Trinidad, West Indies
| | - M Monguió
- School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
| | - F Moreno
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - O Muñoz
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - M J Mumma
- NASA Goddard Space Flight Center, Astrochemistry Laboratory, Code 693.0, Greenbelt, MD 20771, USA
| | - P Nikolov
- Institute of Astronomy and National Astronomical Observatory, 72 Tsarigradsko Chaussée Boulevard, BG-1784 Sofia, Bulgaria
| | - C Opitom
- Institut d'Astrophysique et de Géophysique, Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
- European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
| | - J L Ortiz
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - L Paganini
- NASA Goddard Space Flight Center, Astrochemistry Laboratory, Code 693.0, Greenbelt, MD 20771, USA
| | - M Pajuelo
- IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Lille, France
- Sección Física, Departamento de Ciencias, Pontificia Universidad Católica del Perú, Apartado 1761, Lima, Perú
| | - F J Pozuelos
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
- Institut d'Astrophysique et de Géophysique, Université de Liège, allée du 6 Août 17, 4000 Liège, Belgium
| | - S Protopapa
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - T Pursimo
- Nordic Optical Telescope, Apartado 474, 38700 Santa Cruz de La Palma, Santa Cruz de Tenerife, Spain
| | - B Rajkumar
- Department of Physics, University of the West Indies, St Augustine, Trinidad, West Indies
| | - Y Ramanjooloo
- Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - E Ramos
- Centro Astronómico Hispano-Alemán, Calar Alto, CSIC-MPG, Sierra de los Filabres-04550 Gérgal (Almería), Spain
| | - C Ries
- University Observatory, Ludwig-Maximilian-University Munich, Scheiner Strasse 1, 81679 Munich, Germany
| | - A Riffeser
- University Observatory, Ludwig-Maximilian-University Munich, Scheiner Strasse 1, 81679 Munich, Germany
| | - V Rosenbush
- Main Astronomical Observatory of National Academy of Sciences, Kyiv, UKraine
| | - P Rousselot
- University of Franche-Comté, Observatoire des Sciences de l'Univers THETA, Institut UTINAM - UMR CNRS 6213, BP 1615, 25010 Besançon Cedex, France
| | - E L Ryan
- SETI Institute, 189 Bernardo Avenue Suite 200, Mountain View, CA 94043, USA
| | - P Santos-Sanz
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - D G Schleicher
- Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff, AZ 86001, USA
| | - M Schmidt
- University Observatory, Ludwig-Maximilian-University Munich, Scheiner Strasse 1, 81679 Munich, Germany
| | - R Schulz
- Scientific Support Office, European Space Agency, 2201 AZ Noordwijk, The Netherlands
| | - A K Sen
- Department of Physics, Assam University, Silchar 788011, India
| | - A Somero
- Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
| | - A Sota
- Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - A Stinson
- Armagh Observatory, College Hill, Armagh BT61 9DG, UK
| | - J M Sunshine
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - A Thompson
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast BT7 1NN, UK
| | - G P Tozzi
- INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50 125 Firenze, Italy
| | - C Tubiana
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - G L Villanueva
- NASA Goddard Space Flight Center, Astrochemistry Laboratory, Code 693.0, Greenbelt, MD 20771, USA
| | - X Wang
- Yunnan Observatories, CAS, China, PO Box 110, Kunming 650011, Yunnan Province, People's Republic of China
- Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, Kunming 650011, People's Republic of China
| | - D H Wooden
- NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035-1000, USA
| | - M Yagi
- National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan
| | - B Yang
- European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
| | - B Zaprudin
- Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
| | - T J Zegmott
- Centre for Astrophysics and Planetary Science, School of Physical Sciences, The University of Kent, Canterbury CT2 7NH, UK
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Taylor MGGT, Altobelli N, Buratti BJ, Choukroun M. The Rosetta mission orbiter science overview: the comet phase. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2016.0262. [PMID: 28554981 PMCID: PMC5454230 DOI: 10.1098/rsta.2016.0262] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 03/07/2017] [Indexed: 05/11/2023]
Abstract
The international Rosetta mission was launched in 2004 and consists of the orbiter spacecraft Rosetta and the lander Philae. The aim of the mission is to map the comet 67P/Churyumov-Gerasimenko by remote sensing, and to examine its environment in situ and its evolution in the inner Solar System. Rosetta was the first spacecraft to rendezvous with and orbit a comet, accompanying it as it passes through the inner Solar System, and to deploy a lander, Philae, and perform in situ science on the comet's surface. The primary goals of the mission were to: characterize the comet's nucleus; examine the chemical, mineralogical and isotopic composition of volatiles and refractories; examine the physical properties and interrelation of volatiles and refractories in a cometary nucleus; study the development of cometary activity and the processes in the surface layer of the nucleus and in the coma; detail the origin of comets, the relationship between cometary and interstellar material and the implications for the origin of the Solar System; and characterize asteroids 2867 Steins and 21 Lutetia. This paper presents a summary of mission operations and science, focusing on the Rosetta orbiter component of the mission during its comet phase, from early 2014 up to September 2016.This article is part of the themed issue 'Cometary science after Rosetta'.
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Affiliation(s)
| | - N Altobelli
- ESA/ESAC, 28692 Villanueva de la Cañada, Spain
| | - B J Buratti
- JPL/California Institute of Technology, Pasadena, CA 91109, USA
| | - M Choukroun
- JPL/California Institute of Technology, Pasadena, CA 91109, USA
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Wright IP, Sheridan S, Morgan GH, Barber SJ, Morse AD. On the attempts to measure water (and other volatiles) directly at the surface of a comet. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2015.0385. [PMID: 28416724 PMCID: PMC5394252 DOI: 10.1098/rsta.2015.0385] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 12/14/2016] [Indexed: 05/23/2023]
Abstract
The Ptolemy instrument on the Philae lander (of the Rosetta space mission) was able to make measurements of the major volatiles, water, carbon monoxide and carbon dioxide, directly at the surface of comet 67P/Churyumov-Gerasimenko. We give some background to the mission and highlight those instruments that have already given insights into the notion of water in comets, and which will continue to do so as more results are either acquired or more fully interpreted. On the basis of our results, we show how comets may in fact be heterogeneous over their surface, and how surface measurements can be used in a quest to comprehend the daily cycles of processes that affect the evolution of comets.This article is part of the themed issue 'The origin, history and role of water in the evolution of the inner Solar System'.
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Affiliation(s)
- I P Wright
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - S Sheridan
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - G H Morgan
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - S J Barber
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - A D Morse
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
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20
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Karouia F, Peyvan K, Pohorille A. Toward biotechnology in space: High-throughput instruments for in situ biological research beyond Earth. Biotechnol Adv 2017; 35:905-932. [PMID: 28433608 DOI: 10.1016/j.biotechadv.2017.04.003] [Citation(s) in RCA: 26] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/20/2016] [Revised: 03/27/2017] [Accepted: 04/12/2017] [Indexed: 12/18/2022]
Abstract
Space biotechnology is a nascent field aimed at applying tools of modern biology to advance our goals in space exploration. These advances rely on our ability to exploit in situ high throughput techniques for amplification and sequencing DNA, and measuring levels of RNA transcripts, proteins and metabolites in a cell. These techniques, collectively known as "omics" techniques have already revolutionized terrestrial biology. A number of on-going efforts are aimed at developing instruments to carry out "omics" research in space, in particular on board the International Space Station and small satellites. For space applications these instruments require substantial and creative reengineering that includes automation, miniaturization and ensuring that the device is resistant to conditions in space and works independently of the direction of the gravity vector. Different paths taken to meet these requirements for different "omics" instruments are the subjects of this review. The advantages and disadvantages of these instruments and technological solutions and their level of readiness for deployment in space are discussed. Considering that effects of space environments on terrestrial organisms appear to be global, it is argued that high throughput instruments are essential to advance (1) biomedical and physiological studies to control and reduce space-related stressors on living systems, (2) application of biology to life support and in situ resource utilization, (3) planetary protection, and (4) basic research about the limits on life in space. It is also argued that carrying out measurements in situ provides considerable advantages over the traditional space biology paradigm that relies on post-flight data analysis.
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Affiliation(s)
- Fathi Karouia
- University of California San Francisco, Department of Pharmaceutical Chemistry, San Francisco, CA 94158, USA; NASA Ames Research Center, Exobiology Branch, MS239-4, Moffett Field, CA 94035, USA; NASA Ames Research Center, Flight Systems Implementation Branch, Moffett Field, CA 94035, USA.
| | | | - Andrew Pohorille
- University of California San Francisco, Department of Pharmaceutical Chemistry, San Francisco, CA 94158, USA; NASA Ames Research Center, Exobiology Branch, MS239-4, Moffett Field, CA 94035, USA.
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21
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Filacchione G, Raponi A, Capaccioni F, Ciarniello M, Tosi F, Capria MT, De Sanctis MC, Migliorini A, Piccioni G, Cerroni P, Barucci MA, Fornasier S, Schmitt B, Quirico E, Erard S, Bockelee-Morvan D, Leyrat C, Arnold G, Mennella V, Ammannito E, Bellucci G, Benkhoff J, Bibring JP, Blanco A, Blecka MI, Carlson R, Carsenty U, Colangeli L, Combes M, Combi M, Crovisier J, Drossart P, Encrenaz T, Federico C, Fink U, Fonti S, Fulchignoni M, Ip WH, Irwin P, Jaumann R, Kuehrt E, Langevin Y, Magni G, McCord T, Moroz L, Mottola S, Palomba E, Schade U, Stephan K, Taylor F, Tiphene D, Tozzi GP, Beck P, Biver N, Bonal L, Combe JP, Despan D, Flamini E, Formisano M, Frigeri A, Grassi D, Gudipati MS, Kappel D, Longobardo A, Mancarella F, Markus K, Merlin F, Orosei R, Rinaldi G, Cartacci M, Cicchetti A, Hello Y, Henry F, Jacquinod S, Reess JM, Noschese R, Politi R, Peter G. Seasonal exposure of carbon dioxide ice on the nucleus of comet 67P/Churyumov-Gerasimenko. Science 2016; 354:1563-1566. [DOI: 10.1126/science.aag3161] [Citation(s) in RCA: 49] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/08/2016] [Accepted: 10/28/2016] [Indexed: 11/02/2022]
Affiliation(s)
- G. Filacchione
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Raponi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - F. Capaccioni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. Ciarniello
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - F. Tosi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. T. Capria
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. C. De Sanctis
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Migliorini
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - G. Piccioni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - P. Cerroni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. A. Barucci
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - S. Fornasier
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - B. Schmitt
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - E. Quirico
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - S. Erard
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - D. Bockelee-Morvan
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - C. Leyrat
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - G. Arnold
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - V. Mennella
- INAF Osservatorio di Capodimonte, Naples, Italy
| | - E. Ammannito
- Department of Earth, Planetary, and Space Sciences, University of California–Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - G. Bellucci
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - J. Benkhoff
- ESA (European Space Agency), European Space Research and Technology Centre, Noordwjik, Netherlands
| | - J. P. Bibring
- Institut d’Astrophysique Spatial, CNRS, Orsay, France
| | - A. Blanco
- Dipartimento di Matematica e Fisica “Ennio De Giorgi,” Università del Salento, Lecce, Italy
| | - M. I. Blecka
- Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
| | - R. Carlson
- NASA JPL (Jet Propulsion Laboratory), California Institute of Technology, Pasadena, CA 91109, USA
| | - U. Carsenty
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - L. Colangeli
- ESA (European Space Agency), European Space Research and Technology Centre, Noordwjik, Netherlands
| | - M. Combes
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - M. Combi
- Space Physics Research Laboratory, The University of Michigan, Ann Arbor, MI 48109, USA
| | - J. Crovisier
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - P. Drossart
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - T. Encrenaz
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | | | - U. Fink
- Lunar Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - S. Fonti
- Dipartimento di Matematica e Fisica “Ennio De Giorgi,” Università del Salento, Lecce, Italy
| | - M. Fulchignoni
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - W.-H. Ip
- National Central University, Taipei, Taiwan
| | - P. Irwin
- Departement of Physics, Oxford University, Oxford, UK
| | - R. Jaumann
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - E. Kuehrt
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - Y. Langevin
- Institut d’Astrophysique Spatial, CNRS, Orsay, France
| | - G. Magni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - T. McCord
- Bear Fight Institute, Winthrop, WA 98862, USA
| | - L. Moroz
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - S. Mottola
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - E. Palomba
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - U. Schade
- Helmholtz-Zentrum Berlin für Materialien und Energie, Berlin, Germany
| | - K. Stephan
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - F. Taylor
- Departement of Physics, Oxford University, Oxford, UK
| | - D. Tiphene
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - G. P. Tozzi
- INAF Osservatorio Astrofisico di Arcetri, Firenze, Italy
| | - P. Beck
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - N. Biver
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - L. Bonal
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | | | - D. Despan
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | | | - M. Formisano
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Frigeri
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - D. Grassi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. S. Gudipati
- NASA JPL (Jet Propulsion Laboratory), California Institute of Technology, Pasadena, CA 91109, USA
| | - D. Kappel
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - A. Longobardo
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - F. Mancarella
- Dipartimento di Matematica e Fisica “Ennio De Giorgi,” Università del Salento, Lecce, Italy
| | - K. Markus
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - F. Merlin
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - R. Orosei
- INAF Istituto di Radioastronomia, Bologna, Italy
| | - G. Rinaldi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. Cartacci
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Cicchetti
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - Y. Hello
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - F. Henry
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - S. Jacquinod
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - J. M. Reess
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - R. Noschese
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - R. Politi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - G. Peter
- Institute of Optical Sensor Systems, DLR, Berlin, Germany
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Dehant V, Asael D, Baland RM, Baludikay BK, Beghin J, Belza J, Beuthe M, Breuer D, Chernonozhkin S, Claeys P, Cornet Y, Cornet L, Coyette A, Debaille V, Delvigne C, Deproost MH, De WInter N, Duchemin C, El Atrassi F, François C, De Keyser J, Gillmann C, Gloesener E, Goderis S, Hidaka Y, Höning D, Huber M, Hublet G, Javaux EJ, Karatekin Ö, Kodolanyi J, Revilla LL, Maes L, Maggiolo R, Mattielli N, Maurice M, McKibbin S, Morschhauser A, Neumann W, Noack L, Pham LBS, Pittarello L, Plesa AC, Rivoldini A, Robert S, Rosenblatt P, Spohn T, Storme JY, Tosi N, Trinh A, Valdes M, Vandaele AC, Vanhaecke F, Van Hoolst T, Van Roosbroek N, Wilquet V, Yseboodt M. PLANET TOPERS: Planets, Tracing the Transfer, Origin, Preservation, and Evolution of their ReservoirS. ORIGINS LIFE EVOL B 2016; 46:369-384. [PMID: 27337974 DOI: 10.1007/s11084-016-9488-z] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/15/2015] [Accepted: 01/21/2016] [Indexed: 11/25/2022]
Abstract
The Interuniversity Attraction Pole (IAP) 'PLANET TOPERS' (Planets: Tracing the Transfer, Origin, Preservation, and Evolution of their Reservoirs) addresses the fundamental understanding of the thermal and compositional evolution of the different reservoirs of planetary bodies (core, mantle, crust, atmosphere, hydrosphere, cryosphere, and space) considering interactions and feedback mechanisms. Here we present the first results after 2 years of project work.
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Affiliation(s)
- V Dehant
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium.
| | - D Asael
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - R M Baland
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | | | - J Beghin
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - J Belza
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
- Universiteit Ghent (Ughent), Ghent, Belgium
| | - M Beuthe
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - D Breuer
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | | | - Ph Claeys
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - Y Cornet
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - L Cornet
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - A Coyette
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - V Debaille
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - C Delvigne
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - M H Deproost
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - N De WInter
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - C Duchemin
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - F El Atrassi
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - C François
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - J De Keyser
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - C Gillmann
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - E Gloesener
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - S Goderis
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - Y Hidaka
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - D Höning
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - M Huber
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - G Hublet
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - E J Javaux
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - Ö Karatekin
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - J Kodolanyi
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | | | - L Maes
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - R Maggiolo
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - N Mattielli
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - M Maurice
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - S McKibbin
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - A Morschhauser
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - W Neumann
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - L Noack
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - L B S Pham
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - L Pittarello
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - A C Plesa
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - A Rivoldini
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - S Robert
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - P Rosenblatt
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - T Spohn
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - J -Y Storme
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - N Tosi
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - A Trinh
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - M Valdes
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - A C Vandaele
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | | | - T Van Hoolst
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | | | - V Wilquet
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - M Yseboodt
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
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23
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Abundant molecular oxygen in the coma of comet 67P/Churyumov-Gerasimenko. Nature 2016; 526:678-81. [PMID: 26511578 DOI: 10.1038/nature15707] [Citation(s) in RCA: 62] [Impact Index Per Article: 7.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/29/2015] [Accepted: 08/18/2015] [Indexed: 11/08/2022]
Abstract
The composition of the neutral gas comas of most comets is dominated by H2O, CO and CO2, typically comprising as much as 95 per cent of the total gas density. In addition, cometary comas have been found to contain a rich array of other molecules, including sulfuric compounds and complex hydrocarbons. Molecular oxygen (O2), however, despite its detection on other icy bodies such as the moons of Jupiter and Saturn, has remained undetected in cometary comas. Here we report in situ measurement of O2 in the coma of comet 67P/Churyumov-Gerasimenko, with local abundances ranging from one per cent to ten per cent relative to H2O and with a mean value of 3.80 ± 0.85 per cent. Our observations indicate that the O2/H2O ratio is isotropic in the coma and does not change systematically with heliocentric distance. This suggests that primordial O2 was incorporated into the nucleus during the comet's formation, which is unexpected given the low upper limits from remote sensing observations. Current Solar System formation models do not predict conditions that would allow this to occur.
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24
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Luspay-Kuti A, Mousis O, Hässig M, Fuselier SA, Lunine JI, Marty B, Mandt KE, Wurz P, Rubin M. The presence of clathrates in comet 67P/Churyumov-Gerasimenko. SCIENCE ADVANCES 2016; 2:e1501781. [PMID: 27152351 PMCID: PMC4846445 DOI: 10.1126/sciadv.1501781] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/07/2015] [Accepted: 03/02/2016] [Indexed: 05/25/2023]
Abstract
Cometary nuclei are considered to most closely reflect the composition of the building blocks of our solar system. As such, comets carry important information about the prevalent conditions in the solar nebula before and after planet formation. Recent measurements of the time variation of major and minor volatile species in the coma of the Jupiter family comet 67P/Churyumov-Gerasimenko (67P) by the ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) instrument onboard Rosetta provide insight into the possible origin of this comet. The observed outgassing pattern indicates that the nucleus of 67P contains crystalline ice, clathrates, and other ices. The observed outgassing is not consistent with gas release from an amorphous ice phase with trapped volatile gases. If the building blocks of 67P were formed from crystalline ices and clathrates, then 67P would have agglomerated from ices that were condensed and altered in the protosolar nebula closer to the Sun instead of more pristine ices originating from the interstellar medium or the outskirts of the disc, where amorphous ice may dominate.
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Affiliation(s)
- Adrienn Luspay-Kuti
- Department of Space Research, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA
| | - Olivier Mousis
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, 13388 Marseille, France
| | - Myrtha Hässig
- Department of Space Research, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Stephen A. Fuselier
- Department of Space Research, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA
- Department of Physics and Astronomy, University of Texas at San Antonio, 1 UTSA Circle, San Antonio, TX 78249, USA
| | - Jonathan I. Lunine
- Cornell Center for Astrophysics and Planetary Science, Space Sciences Building Cornell University, Ithaca, NY 14853, USA
| | - Bernard Marty
- CRPG-CNRS, Nancy-Université, 15 rue Notre Dame des Pauvres, 54501 Vandoeuvre-lès-Nancy, France
| | - Kathleen E. Mandt
- Department of Space Research, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA
- Department of Physics and Astronomy, University of Texas at San Antonio, 1 UTSA Circle, San Antonio, TX 78249, USA
| | - Peter Wurz
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, CH-3012 Bern, Switzerland
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
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HIGH-TIME RESOLUTION IN SITU INVESTIGATION OF MAJOR COMETARY VOLATILES AROUND 67P/C–G AT 3.1–2.3 au MEASURED WITH ROSINA-RTOF. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/819/2/126] [Citation(s) in RCA: 28] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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26
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A PROTOSOLAR NEBULA ORIGIN FOR THE ICES AGGLOMERATED BY COMET 67P/CHURYUMOV–GERASIMENKO. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/2041-8205/819/2/l33] [Citation(s) in RCA: 36] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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27
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Exposed water ice on the nucleus of comet 67P/Churyumov-Gerasimenko. Nature 2016; 529:368-72. [PMID: 26760209 DOI: 10.1038/nature16190] [Citation(s) in RCA: 29] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/08/2015] [Accepted: 10/28/2015] [Indexed: 11/08/2022]
Abstract
Although water vapour is the main species observed in the coma of comet 67P/Churyumov-Gerasimenko and water is the major constituent of cometary nuclei, limited evidence for exposed water-ice regions on the surface of the nucleus has been found so far. The absence of large regions of exposed water ice seems a common finding on the surfaces of many of the comets observed so far. The nucleus of 67P/Churyumov-Gerasimenko appears to be fairly uniformly coated with dark, dehydrated, refractory and organic-rich material. Here we report the identification at infrared wavelengths of water ice on two debris falls in the Imhotep region of the nucleus. The ice has been exposed on the walls of elevated structures and at the base of the walls. A quantitative derivation of the abundance of ice in these regions indicates the presence of millimetre-sized pure water-ice grains, considerably larger than in all previous observations. Although micrometre-sized water-ice grains are the usual result of vapour recondensation in ice-free layers, the occurrence of millimetre-sized grains of pure ice as observed in the Imhotep debris falls is best explained by grain growth by vapour diffusion in ice-rich layers, or by sintering. As a consequence of these processes, the nucleus can develop an extended and complex coating in which the outer dehydrated crust is superimposed on layers enriched in water ice. The stratigraphy observed on 67P/Churyumov-Gerasimenko is therefore the result of evolutionary processes affecting the uppermost metres of the nucleus and does not necessarily require a global layering to have occurred at the time of the comet's formation.
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28
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Cessateur G, Keyser JD, Maggiolo R, Gibbons A, Gronoff G, Gunell H, Dhooghe F, Loreau J, Vaeck N, Altwegg K, Bieler A, Briois C, Calmonte U, Combi MR, Fiethe B, Fuselier SA, Gombosi TI, Hässig M, Le Roy L, Neefs E, Rubin M, Sémon T. Photochemistry of forbidden oxygen lines in the inner coma of 67P/Churyumov-Gerasimenko. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2016; 121:804-816. [PMID: 27134807 PMCID: PMC4845638 DOI: 10.1002/2015ja022013] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/07/2015] [Revised: 12/01/2015] [Accepted: 12/24/2015] [Indexed: 06/04/2023]
Abstract
Observations of the green and red-doublet emission lines have previously been realized for several comets. We present here a chemistry-emission coupled model to study the production and loss mechanisms of the O(1S) and O(1D) states, which are responsible for the emission lines of interest for comet 67P/Churyumov-Gerasimenko. The recent discovery of O2 in significant abundance relative to water 3.80 ± 0.85% within the coma of 67P has been taken into consideration for the first time in such models. We evaluate the effect of the presence of O2 on the green to red-doublet emission intensity ratio, which is traditionally used to assess the CO2 abundance within cometary atmospheres. Model simulations, solving the continuity equation with transport, show that not taking O2 into account leads to an underestimation of the CO2 abundance within 67P, with a relative error of about 25%. This strongly suggests that the green to red-doublet emission intensity ratio alone is not a proper tool for determining the CO2 abundance, as previously suggested. Indeed, there is no compelling reason why O2 would not be a common cometary volatile, making revision of earlier assessments regarding the CO2 abundance in cometary atmospheres necessary. The large uncertainties of the CO2 photodissociation cross section imply that more studies are required in order to better constrain the O(1S) and O(1D) production through this mechanism. Space weather phenomena, such as powerful solar flares, could be used as tools for doing so, providing additional information on a good estimation of the O2 abundance within cometary atmospheres.
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Affiliation(s)
- G. Cessateur
- Space Physics DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
| | - J. De Keyser
- Space Physics DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
- Center for Plasma AstrophysicsKatholieke Universiteit LeuvenHeverleeBelgium
| | - R. Maggiolo
- Space Physics DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
| | - A. Gibbons
- Space Physics DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
- Service de Chimie Quantique et PhotophysiqueUniversité Libre de BruxellesBrusselsBelgium
| | - G. Gronoff
- Science Directorate, Chemistry and Dynamics BranchNASA Langley Research CenterHamptonVirginiaUSA
- SSAIHamptonVirginiaUSA
| | - H. Gunell
- Space Physics DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
| | - F. Dhooghe
- Space Physics DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
| | - J. Loreau
- Service de Chimie Quantique et PhotophysiqueUniversité Libre de BruxellesBrusselsBelgium
| | - N. Vaeck
- Service de Chimie Quantique et PhotophysiqueUniversité Libre de BruxellesBrusselsBelgium
| | - K. Altwegg
- Physikalisches InstitutUniversity of BernBernSwitzerland
- Center for Space and HabitabilityUniversity of BernBernSwitzerland
| | - A. Bieler
- Physikalisches InstitutUniversity of BernBernSwitzerland
- Department of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMichiganUSA
| | - C. Briois
- Laboratoire de Physique et Chimie de l'Environnement et de l'EspaceUMR 7328 CNRS, Université dOrléansOrléansFrance
| | - U. Calmonte
- Physikalisches InstitutUniversity of BernBernSwitzerland
| | - M. R. Combi
- Department of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMichiganUSA
| | - B. Fiethe
- Institute of Computer and Network Engineering (IDA)TU BraunschweigBraunschweigGermany
| | - S. A. Fuselier
- Space Science DivisionSouthwest Research InstituteSan AntonioTexasUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTexasUSA
| | - T. I. Gombosi
- Department of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMichiganUSA
| | - M. Hässig
- Physikalisches InstitutUniversity of BernBernSwitzerland
- Space Science DivisionSouthwest Research InstituteSan AntonioTexasUSA
| | - L. Le Roy
- Physikalisches InstitutUniversity of BernBernSwitzerland
| | - E. Neefs
- Engineering DivisionRoyal Belgian Institute for Space AeronomyBrusselsBelgium
| | - M. Rubin
- Physikalisches InstitutUniversity of BernBernSwitzerland
| | - T. Sémon
- Physikalisches InstitutUniversity of BernBernSwitzerland
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29
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Balsiger H, Altwegg K, Bar-Nun A, Berthelier JJ, Bieler A, Bochsler P, Briois C, Calmonte U, Combi M, De Keyser J, Eberhardt P, Fiethe B, Fuselier SA, Gasc S, Gombosi TI, Hansen KC, Hässig M, Jäckel A, Kopp E, Korth A, Le Roy L, Mall U, Marty B, Mousis O, Owen T, Rème H, Rubin M, Sémon T, Tzou CY, Waite JH, Wurz P. Detection of argon in the coma of comet 67P/Churyumov-Gerasimenko. SCIENCE ADVANCES 2015; 1:e1500377. [PMID: 26601264 PMCID: PMC4643765 DOI: 10.1126/sciadv.1500377] [Citation(s) in RCA: 13] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/25/2015] [Accepted: 06/22/2015] [Indexed: 05/15/2023]
Abstract
Comets have been considered to be representative of icy planetesimals that may have contributed a significant fraction of the volatile inventory of the terrestrial planets. For example, comets must have brought some water to Earth. However, the magnitude of their contribution is still debated. We report the detection of argon and its relation to the water abundance in the Jupiter family comet 67P/Churyumov-Gerasimenko by in situ measurement of the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) mass spectrometer aboard the Rosetta spacecraft. Despite the very low intensity of the signal, argon is clearly identified by the exact determination of the mass of the isotope (36)Ar and by the (36)Ar/(38)Ar ratio. Because of time variability and spatial heterogeneity of the coma, only a range of the relative abundance of argon to water can be given. Nevertheless, this range confirms that comets of the type 67P/Churyumov-Gerasimenko cannot be the major source of Earth's major volatiles.
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Affiliation(s)
- Hans Balsiger
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Corresponding author:
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Akiva Bar-Nun
- Department of Geoscience, Tel Aviv University, Ramat Aviv, Tel Aviv 69978, Israel
| | - Jean-Jacques Berthelier
- LATMOS (Laboratoire Atmosphères, Milieux, Observations Spatiales)/IPSL (Institut Pierre Simon Laplace)–CNRS–UPMC (University Pierre et Marie Curie)–UVSQ (Université de Versailles Saint-Quentin-en-Yvelines), 4 Avenue de Neptune, F-94100 Saint-Maur, France
| | - Andre Bieler
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Peter Bochsler
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Christelle Briois
- Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E), UMR 6115 CNRS–Université d’Orléans, 45071 Orléans, France
| | - Ursina Calmonte
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Michael Combi
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Johan De Keyser
- Belgian Institute for Space Aeronomy (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium
| | - Peter Eberhardt
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Björn Fiethe
- Institute of Computer and Network Engineering (IDA), Technische Universität (TU) Braunschweig, Hans-Sommer-Straße 66, D-38106 Braunschweig, Germany
| | - Stephen A. Fuselier
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - Sébastien Gasc
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Tamas I. Gombosi
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Kenneth C. Hansen
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - Myrtha Hässig
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - Annette Jäckel
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Ernest Kopp
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Axel Korth
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Lena Le Roy
- Center for Space and Habitability, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Urs Mall
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Bernard Marty
- CRPG (Centre de Recherches Pétrographiques et Géochimiques)–CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre lès Nancy, France
| | - Olivier Mousis
- Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
| | - Tobias Owen
- Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
| | - Henri Rème
- Université de Toulouse; UPS (Université Paul Sabatier)–OMP (L’Observatoire Midi-Pyrénées); IRAP (L’Institut de Recherche en Astrophysique et Planétologie), 31400 Toulouse, France
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Thierry Sémon
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Chia-Yu Tzou
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - J. Hunter Waite
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - Peter Wurz
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
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Wright IP, Sheridan S, Barber SJ, Morgan GH, Andrews DJ, Morse AD. CHO-bearing organic compounds at the surface of 67P/Churyumov-Gerasimenko revealed by Ptolemy. Science 2015; 349:aab0673. [DOI: 10.1126/science.aab0673] [Citation(s) in RCA: 92] [Impact Index Per Article: 10.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- I. P. Wright
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - S. Sheridan
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - S. J. Barber
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - G. H. Morgan
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - D. J. Andrews
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
| | - A. D. Morse
- Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
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31
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Goesmann F, Rosenbauer H, Bredehoft JH, Cabane M, Ehrenfreund P, Gautier T, Giri C, Kruger H, Le Roy L, MacDermott AJ, McKenna-Lawlor S, Meierhenrich UJ, Caro GMM, Raulin F, Roll R, Steele A, Steininger H, Sternberg R, Szopa C, Thiemann W, Ulamec S. Organic compounds on comet 67P/Churyumov-Gerasimenko revealed by COSAC mass spectrometry. Science 2015; 349:aab0689. [DOI: 10.1126/science.aab0689] [Citation(s) in RCA: 326] [Impact Index Per Article: 36.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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32
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Rubin M, Altwegg K, Balsiger H, Bar-Nun A, Berthelier JJ, Bieler A, Bochsler P, Briois C, Calmonte U, Combi M, De Keyser J, Dhooghe F, Eberhardt P, Fiethe B, Fuselier SA, Gasc S, Gombosi TI, Hansen KC, Hässig M, Jäckel A, Kopp E, Korth A, Le Roy L, Mall U, Marty B, Mousis O, Owen T, Rème H, Sémon T, Tzou CY, Waite JH, Wurz P. Molecular nitrogen in comet 67P/Churyumov-Gerasimenko indicates a low formation temperature. Science 2015; 348:232-5. [PMID: 25791084 DOI: 10.1126/science.aaa6100] [Citation(s) in RCA: 176] [Impact Index Per Article: 19.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/12/2015] [Accepted: 03/03/2015] [Indexed: 11/02/2022]
Abstract
Molecular nitrogen (N2) is thought to have been the most abundant form of nitrogen in the protosolar nebula. It is the main N-bearing molecule in the atmospheres of Pluto and Triton and probably the main nitrogen reservoir from which the giant planets formed. Yet in comets, often considered the most primitive bodies in the solar system, N2 has not been detected. Here we report the direct in situ measurement of N2 in the Jupiter family comet 67P/Churyumov-Gerasimenko, made by the Rosetta Orbiter Spectrometer for Ion and Neutral Analysis mass spectrometer aboard the Rosetta spacecraft. A N2/CO ratio of (5.70 ± 0.66) × 10(-3) (2σ standard deviation of the sampled mean) corresponds to depletion by a factor of ~25.4 ± 8.9 as compared to the protosolar value. This depletion suggests that cometary grains formed at low-temperature conditions below ~30 kelvin.
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Affiliation(s)
- M Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland.
| | - K Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Center for Space and Habitability, University of Bern, Sidlerstrasse. 5, CH-3012 Bern, Switzerland
| | - H Balsiger
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - A Bar-Nun
- Department of Geoscience, Tel-Aviv University, Ramat-Aviv, Tel-Aviv, Israel
| | - J-J Berthelier
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS)/Institute Pierre Simon Laplace-CNRS-UPMC-UVSQ, 4 Avenue de Neptune F-94100, Saint-Maur, France
| | - A Bieler
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - P Bochsler
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - C Briois
- Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), UMR 6115 CNRS-Université d'Orléans, Orléans, France
| | - U Calmonte
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - M Combi
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - J De Keyser
- Belgian Institute for Space Aeronomy, Belgisch Instituut voor Ruimte-Aeronomie-Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium
| | - F Dhooghe
- Belgian Institute for Space Aeronomy, Belgisch Instituut voor Ruimte-Aeronomie-Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium
| | - P Eberhardt
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - B Fiethe
- Institute of Computer and Network Engineering, Technische Universität Braunschweig, Hans-Sommer-Straße 66, D-38106 Braunschweig, Germany
| | - S A Fuselier
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - S Gasc
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - T I Gombosi
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - K C Hansen
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward, Ann Arbor, MI 48109, USA
| | - M Hässig
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland. Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - A Jäckel
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - E Kopp
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - A Korth
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - L Le Roy
- Center for Space and Habitability, University of Bern, Sidlerstrasse. 5, CH-3012 Bern, Switzerland
| | - U Mall
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - B Marty
- Centre de Recherches Pétrographiques et Géochimiques (CRPG)-CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, Bôite Postale 20, 54501 Vandoeuvre lès Nancy, France
| | - O Mousis
- Aix Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille UMR 7326, 13388, Marseille, France
| | - T Owen
- Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
| | - H Rème
- Université de Toulouse; UPS-OMP; Institut de Recherche en Astrophysique et Planétologie (IRAP), Toulouse, France. CNRS; IRAP; 9 Avenue du Colonel Roche, Boîte Postale 44346, F-31028 Toulouse Cedex 4, France
| | - T Sémon
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - C-Y Tzou
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - J H Waite
- Department of Space Science, Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228, USA
| | - P Wurz
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
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Sierks H, Barbieri C, Lamy PL, Rodrigo R, Koschny D, Rickman H, Keller HU, Agarwal J, A'Hearn MF, Angrilli F, Auger AT, Barucci MA, Bertaux JL, Bertini I, Besse S, Bodewits D, Capanna C, Cremonese G, Da Deppo V, Davidsson B, Debei S, De Cecco M, Ferri F, Fornasier S, Fulle M, Gaskell R, Giacomini L, Groussin O, Gutierrez-Marques P, Gutiérrez PJ, Güttler C, Hoekzema N, Hviid SF, Ip WH, Jorda L, Knollenberg J, Kovacs G, Kramm JR, Kührt E, Küppers M, La Forgia F, Lara LM, Lazzarin M, Leyrat C, Lopez Moreno JJ, Magrin S, Marchi S, Marzari F, Massironi M, Michalik H, Moissl R, Mottola S, Naletto G, Oklay N, Pajola M, Pertile M, Preusker F, Sabau L, Scholten F, Snodgrass C, Thomas N, Tubiana C, Vincent JB, Wenzel KP, Zaccariotto M, Pätzold M. Cometary science. On the nucleus structure and activity of comet 67P/Churyumov-Gerasimenko. Science 2015; 347:aaa1044. [PMID: 25613897 DOI: 10.1126/science.aaa1044] [Citation(s) in RCA: 35] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Images from the OSIRIS scientific imaging system onboard Rosetta show that the nucleus of 67P/Churyumov-Gerasimenko consists of two lobes connected by a short neck. The nucleus has a bulk density less than half that of water. Activity at a distance from the Sun of >3 astronomical units is predominantly from the neck, where jets have been seen consistently. The nucleus rotates about the principal axis of momentum. The surface morphology suggests that the removal of larger volumes of material, possibly via explosive release of subsurface pressure or via creation of overhangs by sublimation, may be a major mass loss process. The shape raises the question of whether the two lobes represent a contact binary formed 4.5 billion years ago, or a single body where a gap has evolved via mass loss.
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Affiliation(s)
- Holger Sierks
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany.
| | - Cesare Barbieri
- Department of Physics and Astronomy, University of Padova, 35122 Padova, Italy
| | - Philippe L Lamy
- Laboratoire d'Astrophysique de Marseille, UMR 7326, CNRS & Aix Marseille Université, 13388 Marseille Cedex 13, France
| | - Rafael Rodrigo
- Centro de Astrobiologia, CSIC-INTA,28850 Madrid, Spain. International Space Science Institute, 3012 Bern, Switzerland
| | - Detlef Koschny
- Scientific Support Office, European Space Research and Technology Centre/ESA, 2201 AZ Noordwijk ZH, Netherlands
| | - Hans Rickman
- Department of Physics and Astronomy, Uppsala University, 75120 Uppsala, Sweden. PAS Space Research Center, 00716 Warszawa, Poland
| | - Horst Uwe Keller
- Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, 38106 Braunschweig, Germany. Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Jessica Agarwal
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Michael F A'Hearn
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany. Department of Astronomy, University of Maryland, College Park, MD 20742, USA. Akademie der Wissenschaften zu Göttingen, 37077 Göttingen, Germany
| | - Francesco Angrilli
- Department of Industrial Engineering, University of Padova, 35131 Padova, Italy
| | - Anne-Therese Auger
- Aix Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, 13388 Marseille, France
| | - M Antonella Barucci
- LESIA-Observatoire de Paris, CNRS, Université Pierre et Marie Curie, Université Paris Diderot, 92195 Meudon, France
| | | | - Ivano Bertini
- Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy
| | - Sebastien Besse
- Scientific Support Office, European Space Research and Technology Centre/ESA, 2201 AZ Noordwijk ZH, Netherlands
| | - Dennis Bodewits
- Department of Astronomy, University of Maryland, College Park, MD 20742, USA
| | - Claire Capanna
- Aix Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, 13388 Marseille, France
| | | | | | - Björn Davidsson
- Department of Physics and Astronomy, Uppsala University, 75120 Uppsala, Sweden
| | - Stefano Debei
- Department of Industrial Engineering, University of Padova, 35131 Padova, Italy
| | | | - Francesca Ferri
- Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy
| | - Sonia Fornasier
- LESIA-Observatoire de Paris, CNRS, Université Pierre et Marie Curie, Université Paris Diderot, 92195 Meudon, France
| | - Marco Fulle
- INAF - Osservatorio Astronomico di Trieste, 34014 Trieste, Italy
| | | | - Lorenza Giacomini
- Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy
| | - Olivier Groussin
- Aix Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, 13388 Marseille, France
| | | | - Pedro J Gutiérrez
- Instituto de Astrofisica de Andalucia (CSIC), c/ Glorieta de la AstronomÌa s/n, 18008 Granada, Spain
| | - Carsten Güttler
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Nick Hoekzema
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Stubbe F Hviid
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany. Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Wing-Huen Ip
- Graduate Institute of Astronomy, National Central University, Chung-Li 32054, Taiwan. Space Science Institute, Macau University of Science and Technology, Macao, China
| | - Laurent Jorda
- Aix Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, 13388 Marseille, France
| | - Jörg Knollenberg
- Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Gabor Kovacs
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - J Rainer Kramm
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Ekkehard Kührt
- Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Michael Küppers
- Operations Department, European Space Astronomy Centre/ESA, 28691 Villanueva de la Canada, Madrid, Spain
| | | | - Luisa M Lara
- Instituto de Astrofisica de Andalucia (CSIC), c/ Glorieta de la AstronomÌa s/n, 18008 Granada, Spain
| | - Monica Lazzarin
- Department of Physics and Astronomy, University of Padova, 35122 Padova, Italy
| | - Cédric Leyrat
- LESIA-Observatoire de Paris, CNRS, Université Pierre et Marie Curie, Université Paris Diderot, 92195 Meudon, France
| | - Josè J Lopez Moreno
- Instituto de Astrofisica de Andalucia (CSIC), c/ Glorieta de la AstronomÌa s/n, 18008 Granada, Spain
| | - Sara Magrin
- Department of Physics and Astronomy, University of Padova, 35122 Padova, Italy
| | - Simone Marchi
- Solar System Exploration Research, Virtual Institute, Southwest Research Institute, Boulder, CO 80302, USA
| | - Francesco Marzari
- Department of Physics and Astronomy, University of Padova, 35122 Padova, Italy
| | - Matteo Massironi
- Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy. Dipartimento di Geoscienze, University of Padova, 35131 Padova, Italy
| | - Harald Michalik
- Institut für Datentechnik und Kommunikationsnetze der TU Braunschweig, 38106 Braunschweig, Germany
| | - Richard Moissl
- Operations Department, European Space Astronomy Centre/ESA, 28691 Villanueva de la Canada, Madrid, Spain
| | - Stefano Mottola
- Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Giampiero Naletto
- Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy. CNR-IFN UOS Padova LUXOR, 35131 Padova, Italy. Department of Information Engineering, University of Padova, 35131 Padova, Italy
| | - Nilda Oklay
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Maurizio Pajola
- Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy
| | - Marco Pertile
- Department of Industrial Engineering, University of Padova, 35131 Padova, Italy. Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy
| | - Frank Preusker
- Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Lola Sabau
- Instituto Nacional de Tecnica Aeroespacial, 28850 Torrejon de Ardoz, Madrid, Spain
| | - Frank Scholten
- Deutsches Zentrum für Luft- und Raumfahrt, Institut für Planetenforschung, 12489 Berlin, Germany
| | - Colin Snodgrass
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Nicolas Thomas
- Physikalisches Institut, University of Bern, 3012 Bern, Switzerland. Center for Space and Habitability, University of Bern, 3012 Bern, Switzerland
| | - Cecilia Tubiana
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | | | - Klaus-Peter Wenzel
- Scientific Support Office, European Space Research and Technology Centre/ESA, 2201 AZ Noordwijk ZH, Netherlands
| | - Mirco Zaccariotto
- Department of Industrial Engineering, University of Padova, 35131 Padova, Italy. Centro di Ateneo di Studi ed Attività Spaziali "Giuseppe Colombo" (CISAS), University of Padova, 35131 Padova, Italy
| | - Martin Pätzold
- Rheinisches Institut für Umweltforschung, Abteilung Planetenforschung, Universität zu Köln, 50931 Köln, Germany
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34
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Rotundi A, Sierks H, Della Corte V, Fulle M, Gutierrez PJ, Lara L, Barbieri C, Lamy PL, Rodrigo R, Koschny D, Rickman H, Keller HU, López-Moreno JJ, Accolla M, Agarwal J, A'Hearn MF, Altobelli N, Angrilli F, Barucci MA, Bertaux JL, Bertini I, Bodewits D, Bussoletti E, Colangeli L, Cosi M, Cremonese G, Crifo JF, Da Deppo V, Davidsson B, Debei S, De Cecco M, Esposito F, Ferrari M, Fornasier S, Giovane F, Gustafson B, Green SF, Groussin O, Grün E, Güttler C, Herranz ML, Hviid SF, Ip W, Ivanovski S, Jerónimo JM, Jorda L, Knollenberg J, Kramm R, Kührt E, Küppers M, Lazzarin M, Leese MR, López-Jiménez AC, Lucarelli F, Lowry SC, Marzari F, Epifani EM, McDonnell JAM, Mennella V, Michalik H, Molina A, Morales R, Moreno F, Mottola S, Naletto G, Oklay N, Ortiz JL, Palomba E, Palumbo P, Perrin JM, Rodríguez J, Sabau L, Snodgrass C, Sordini R, Thomas N, Tubiana C, Vincent JB, Weissman P, Wenzel KP, Zakharov V, Zarnecki JC. Cometary science. Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the Sun. Science 2015; 347:aaa3905. [PMID: 25613898 DOI: 10.1126/science.aaa3905] [Citation(s) in RCA: 291] [Impact Index Per Article: 32.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Critical measurements for understanding accretion and the dust/gas ratio in the solar nebula, where planets were forming 4.5 billion years ago, are being obtained by the GIADA (Grain Impact Analyser and Dust Accumulator) experiment on the European Space Agency's Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko. Between 3.6 and 3.4 astronomical units inbound, GIADA and OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) detected 35 outflowing grains of mass 10(-10) to 10(-7) kilograms, and 48 grains of mass 10(-5) to 10(-2) kilograms, respectively. Combined with gas data from the MIRO (Microwave Instrument for the Rosetta Orbiter) and ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) instruments, we find a dust/gas mass ratio of 4 ± 2 averaged over the sunlit nucleus surface. A cloud of larger grains also encircles the nucleus in bound orbits from the previous perihelion. The largest orbiting clumps are meter-sized, confirming the dust/gas ratio of 3 inferred at perihelion from models of dust comae and trails.
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Affiliation(s)
- Alessandra Rotundi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. Università degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy.
| | - Holger Sierks
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - Vincenzo Della Corte
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy
| | - Marco Fulle
- Osservatorio Astronomico, INAF, Via Tiepolo 11, 34143 Trieste, Italy
| | - Pedro J Gutierrez
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Luisa Lara
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Cesare Barbieri
- Department of Physics and Astronomy, Padova University, Vicolo dell'Osservatorio 3, 35122 Padova, Italy
| | - Philippe L Lamy
- Laboratoire d'Astrophysique de Marseille, UMR 7326, CNRS and Aix-Marseille Université, 13388 Marseille, France
| | - Rafael Rodrigo
- Centro de Astrobiologia (Instituto Nacional de Tecnica Aerospacial-CSIC), 28691 Villanueva de la Canada, Madrid, Spain. International Space Science Institute, Hallerstrasse 6, CH-3012 Bern, Switzerland
| | - Detlef Koschny
- Scientific Support Office, European Space Agency, 2201 Noordwijk, Netherlands
| | - Hans Rickman
- Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden. Polish Academy of Sciences Space Research Center, Bartycka 18A, PL-00716 Warszawa, Poland
| | - Horst Uwe Keller
- Institute for Geophysics and Extraterrestrial Physics, Technische Universität Braunschweig, Braunschweig 38106, Germany
| | - José J López-Moreno
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Mario Accolla
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. Università degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy
| | - Jessica Agarwal
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - Michael F A'Hearn
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - Nicolas Altobelli
- European Space Agency (ESA)-European Space Astronomy Center (ESAC), Camino Bajo del Castillo, s/n, 28692 Villanueva de la Cañada, Madrid, Spagna
| | - Francesco Angrilli
- Department of Mechanical Engineering, University of Padova, via Venezia 1, 35131 Padova, Italy
| | - M Antonietta Barucci
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Université Paris 06, Université Paris-Diderot, 5 place Johannes Janssen, 92195 Meudon, France
| | - Jean-Loup Bertaux
- Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS/Université de Versailles Saint-Quentin-en-Yvelines/Institut Pierre-Simon Laplace, 11 boulevard d'Alembert, 78280 Guyancourt, France
| | - Ivano Bertini
- University of Padova, Centro Interdipartimentale di Studi e Attività Spaziali (CISAS), via Venezia 15, 35100 Padova, Italy
| | - Dennis Bodewits
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| | - Ezio Bussoletti
- Università degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy
| | - Luigi Colangeli
- ESA, European Space Research and Technology Centre (ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, Netherlands
| | - Massimo Cosi
- Selex-ES, Via Albert Einstein, 35, 50013 Campi Bisenzio, Firenze, Italy
| | - Gabriele Cremonese
- Osservatorio Astronomico di Padova, INAF, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
| | - Jean-Francois Crifo
- Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS/Université de Versailles Saint-Quentin-en-Yvelines/Institut Pierre-Simon Laplace, 11 boulevard d'Alembert, 78280 Guyancourt, France
| | - Vania Da Deppo
- Consiglio Nazionale delle Ricerche-Istituto di Fotonica e Nanotecnologie-Unità Operativa di Supporto Padova LUXOR, via Trasea 7, 35131 Padova, Italy
| | - Björn Davidsson
- Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden
| | - Stefano Debei
- Department of Mechanical Engineering, University of Padova, via Venezia 1, 35131 Padova, Italy
| | | | - Francesca Esposito
- Osservatorio Astronomico di Capodimonte, INAF, Salita Moiariello, 16, 80133 Naples, Italy
| | - Marco Ferrari
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. Università degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy
| | - Sonia Fornasier
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Université Paris 06, Université Paris-Diderot, 5 place Johannes Janssen, 92195 Meudon, France
| | - Frank Giovane
- Virginia Polytechnic Institute and State University, Blacksburg, VA 24061, USA
| | - Bo Gustafson
- University of Florida, Gainesville, FL 32611, USA
| | - Simon F Green
- Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
| | - Olivier Groussin
- Laboratoire d'Astrophysique de Marseille, UMR 7326, CNRS and Aix-Marseille Université, 13388 Marseille, France
| | - Eberhard Grün
- Max-Planck-Institut fuer Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - Carsten Güttler
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - Miguel L Herranz
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Stubbe F Hviid
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
| | - Wing Ip
- Institute for Space Science, National Central University, 300 Chung Da Road, 32054 Chung-Li, Taiwan
| | - Stavro Ivanovski
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy
| | - José M Jerónimo
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Laurent Jorda
- Laboratoire d'Astrophysique de Marseille, UMR 7326, CNRS and Aix-Marseille Université, 13388 Marseille, France
| | - Joerg Knollenberg
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
| | - Rainer Kramm
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - Ekkehard Kührt
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
| | - Michael Küppers
- European Space Agency (ESA)-European Space Astronomy Center (ESAC), Camino Bajo del Castillo, s/n, 28692 Villanueva de la Cañada, Madrid, Spagna
| | - Monica Lazzarin
- Department of Physics and Astronomy, Padova University, Vicolo dell'Osservatorio 3, 35122 Padova, Italy
| | - Mark R Leese
- Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
| | - Antonio C López-Jiménez
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Francesca Lucarelli
- Università degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy
| | - Stephen C Lowry
- The University of Kent, School of Physical Sciences, Canterbury, Kent CT2 7NZ, UK
| | | | - Elena Mazzotta Epifani
- Osservatorio Astronomico di Capodimonte, INAF, Salita Moiariello, 16, 80133 Naples, Italy
| | - J Anthony M McDonnell
- Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK. The University of Kent, School of Physical Sciences, Canterbury, Kent CT2 7NZ, UK. Unispacekent, Canterbury CT2 8EF, UK
| | - Vito Mennella
- Osservatorio Astronomico di Capodimonte, INAF, Salita Moiariello, 16, 80133 Naples, Italy
| | - Harald Michalik
- Institut für Datentechnik und Kommunikationsnetze, 38106 Braunschweig, Germany
| | - Antonio Molina
- Departamento de Física Aplicada, Universidad de Granada, Facultad de Ciencias, Avenida Severo Ochoa, s/n, 18071 Granada, Spain
| | - Rafael Morales
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Fernando Moreno
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Stefano Mottola
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
| | - Giampiero Naletto
- Department of Information Engineering, Padova University, via Gradenigo 6, 35131 Padova, Italy
| | - Nilda Oklay
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - José L Ortiz
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Ernesto Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy
| | - Pasquale Palumbo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy. Università degli Studi di Napoli "Parthenope," Dipartimento di Scienze e Tecnologie, CDN IC4, 80143 Naples, Italy
| | - Jean-Marie Perrin
- Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS/Université de Versailles Saint-Quentin-en-Yvelines/Institut Pierre-Simon Laplace, 11 boulevard d'Alembert, 78280 Guyancourt, France. Observatoire de Haute Provence OSU Pythéas UMS 2244 CNRS-AMU, 04870 Saint Michel l'Observatoire, France
| | - Julio Rodríguez
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), P.O. Box 3008, 18080 Granada, Spain
| | - Lola Sabau
- Instituto Nacional de Tecnica Aeroespacial, Carretera de Ajalvir, p.k. 4, 28850 Torrejon de Ardoz, Madrid, Spain
| | - Colin Snodgrass
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany. Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
| | - Roberto Sordini
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Via Fosso del Cavaliere, 100, 0133 Rome, Italy
| | - Nicolas Thomas
- Physikalisches Institut, Sidlerstrasse 5, University of Bern, 3012 Bern, Switzerland
| | - Cecilia Tubiana
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - Jean-Baptiste Vincent
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg, 3, 37077 Göttingen, Germany
| | - Paul Weissman
- Planetary Science Section, Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - Klaus-Peter Wenzel
- Scientific Support Office, European Space Agency, 2201 Noordwijk, Netherlands
| | - Vladimir Zakharov
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Université Paris 06, Université Paris-Diderot, 5 place Johannes Janssen, 92195 Meudon, France
| | - John C Zarnecki
- International Space Science Institute, Hallerstrasse 6, CH-3012 Bern, Switzerland. Planetary and Space Sciences, Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
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Gibney E. Science pours in from Rosetta comet mission. Nature 2015. [DOI: 10.1038/nature.2015.16777] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Lu Z, Chang YC, Benitez Y, Luo Z, Houria AB, Ayari T, Al Mogren MM, Hochlaf M, Jackson WM, Ng CY. State-to-state vacuum ultraviolet photodissociation study of CO2 on the formation of state-correlated CO(X1Σ+; v) with O(1D) and O(1S) photoproducts at 11.95–12.22 eV. Phys Chem Chem Phys 2015; 17:11752-62. [PMID: 25868654 DOI: 10.1039/c5cp01321f] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
The state-to-state photodissociation of CO2 is investigated in the VUV range of 11.94–12.20 eV.
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Affiliation(s)
- Zhou Lu
- Department of Chemistry
- University of California
- Davis
- USA
| | | | | | - Zhihong Luo
- Department of Chemistry
- University of California
- Davis
- USA
| | - Adel Ben Houria
- Laboratoire de Spectroscopie Atomique
- Moléculaire et Applications – LSAMA
- Université de Tunis El Manar
- Tunis
- Tunisia
| | - Tarek Ayari
- Laboratoire de Spectroscopie Atomique
- Moléculaire et Applications – LSAMA
- Université de Tunis El Manar
- Tunis
- Tunisia
| | | | - M. Hochlaf
- Université Paris-Est
- Laboratoire Modélisation et Simulation Multi Echelle
- MSME UMR 8208 CNRS
- 77454 Marne-la-Vallée
- France
| | - W. M. Jackson
- Department of Chemistry
- University of California
- Davis
- USA
| | - C. Y. Ng
- Department of Chemistry
- University of California
- Davis
- USA
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