1
|
Marks JH, Bai X, Nikolayev AA, Gong Q, Zhu C, Kleimeier NF, Turner AM, Singh SK, Wang J, Yang J, Pan Y, Yang T, Mebel AM, Kaiser RI. Methanetriol─Formation of an Impossible Molecule. J Am Chem Soc 2024; 146:12174-12184. [PMID: 38629886 DOI: 10.1021/jacs.4c02637] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 05/02/2024]
Abstract
Orthocarboxylic acids─organic molecules carrying three hydroxyl groups at the same carbon atom─have been distinguished as vital reactive intermediates by the atmospheric science and physical (organic) chemistry communities as transients in the atmospheric aerosol cycle. Predicted short lifetimes and their tendency to dehydrate to a carboxylic acid, free orthocarboxylic acids, signify one of the most elusive classes of organic reactive intermediates, with even the simplest representative methanetriol (CH(OH)3)─historically known as orthoformic acid─not previously been detected experimentally. Here, we report the first synthesis of the previously elusive methanetriol molecule in low-temperature mixed methanol (CH3OH) and molecular oxygen (O2) ices subjected to energetic irradiation. Supported by electronic structure calculations, methanetriol was identified in the gas phase upon sublimation via isomer-selective photoionization reflectron time-of-flight mass spectrometry combined with isotopic substitution studies and the detection of photoionization fragments. The first synthesis and detection of methanetriol (CH(OH)3) reveals its gas-phase stability as supported by a significant barrier hindering unimolecular decomposition. These findings progress our fundamental understanding of the chemistry and chemical bonding of methanetriol, hydroxyperoxymethane (CH3OOOH), and hydroxyperoxymethanol (CH2(OH)OOH), which are all prototype molecules in the oxidation chemistry of the atmosphere.
Collapse
Affiliation(s)
- Joshua H Marks
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| | - Xilin Bai
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200062, P. R. China
| | | | - Qi'ang Gong
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200062, P. R. China
| | - Cheng Zhu
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| | - N Fabian Kleimeier
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| | - Andrew M Turner
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| | - Santosh K Singh
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| | - Jia Wang
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| | - Jiuzhong Yang
- National Synchrotron Radiation Laboratory, University of Science and Technology of China, Hefei, Anhui 230029, P. R. China
| | - Yang Pan
- National Synchrotron Radiation Laboratory, University of Science and Technology of China, Hefei, Anhui 230029, P. R. China
| | - Tao Yang
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai 200062, P. R. China
- Collaborative Innovation Center of Extreme Optics, Shanxi University, Taiyuan, Shanxi 030006, P. R. China
| | - Alexander M Mebel
- Department of Chemistry and Biochemistry, Florida International University, Miami, Florida 33199, United States
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
- W. M. Keck Research Laboratory in Astrochemistry, University of Hawaii at Manoa, Honolulu, Hawaii 96822, United States
| |
Collapse
|
2
|
Paschek K, Lee M, Semenov DA, Henning TK. Prebiotic Vitamin B 3 Synthesis in Carbonaceous Planetesimals. Chempluschem 2024; 89:e202300508. [PMID: 37847591 DOI: 10.1002/cplu.202300508] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/08/2023] [Revised: 10/11/2023] [Accepted: 10/12/2023] [Indexed: 10/19/2023]
Abstract
Aqueous chemistry within carbonaceous planetesimals is promising for synthesizing prebiotic organic matter essential to all life. Meteorites derived from these planetesimals delivered these life building blocks to the early Earth, potentially facilitating the origins of life. Here, we studied the formation of vitamin B3 as it is an important precursor of the coenzyme NAD(P)(H), which is essential for the metabolism of all life as we know it. We propose a new reaction mechanism based on known experiments in the literature that explains the synthesis of vitamin B3. It combines the sugar precursors glyceraldehyde or dihydroxyacetone with the amino acids aspartic acid or asparagine in aqueous solution without oxygen or other oxidizing agents. We performed thermochemical equilibrium calculations to test the thermodynamic favorability. The predicted vitamin B3 abundances resulting from this new pathway were compared with measured values in asteroids and meteorites. We conclude that competition for reactants and decomposition by hydrolysis are necessary to explain the prebiotic content of meteorites. In sum, our model fits well into the complex network of chemical pathways active in this environment.
Collapse
Affiliation(s)
- Klaus Paschek
- Max Planck Institute for Astronomy, Königstuhl 17, D-69117, Heidelberg, Germany
| | - Mijin Lee
- Max Planck Institute for Astronomy, Königstuhl 17, D-69117, Heidelberg, Germany
| | - Dmitry A Semenov
- Max Planck Institute for Astronomy, Königstuhl 17, D-69117, Heidelberg, Germany
- Department of Chemistry, Ludwig Maximilian University of Munich, Butenandtstraße 5-13, House F, D-81377, Munich, Germany
| | - Thomas K Henning
- Max Planck Institute for Astronomy, Königstuhl 17, D-69117, Heidelberg, Germany
| |
Collapse
|
3
|
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.
Collapse
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
| |
Collapse
|
4
|
Garrett NR, Davis MC, Fortenberry RC. DFT + F12 QFFs for Cost-Effective Rovibrational Spectral Data Predictions of Ground and Excited Electronic States. J Chem Theory Comput 2024. [PMID: 38230913 DOI: 10.1021/acs.jctc.3c01179] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/18/2024]
Abstract
The quest for faster computation of anharmonic vibrational frequencies of both ground and excited electronic states has led to combining coupled cluster theory harmonic force constants with density functional theory cubic and quartic force constants for defining a quartic force field (QFF) utilized in conjunction with vibrational perturbation theory at second order (VPT2). This work shows that explicitly correlated coupled cluster theory at the singles, doubles, and perturbative triples levels [CCSD(T)-F12] provides accurate anharmonic vibrational frequencies and rotational constants when conjoined with any of B3LYP, CAM-B3LYP, BHandHLYP, PBE0, and ωB97XD for roughly one-quarter of the computational time of the CCSD(T)-F12 QFF alone for our test set. As the number of atoms in the molecule increases, however, the anharmonic terms become a greater portion of the QFF, and the cost comparison improves with HOCO+ and formic acid, requiring less than 15 and 10% of the time, respectively. In electronically excited states, PBE0 produces more consistently accurate results. Additionally, as the size of the molecule and, in turn, QFF increase, the cost savings for utilizing such a hybrid approach for both ground- and excited-state computations grows. As such, these methods are promising for predicting accurate rovibrational spectral properties for electronically excited states. In cases where well-behaved potentials for a small selection of targeted excited states are needed, such an approach should reduce the computational cost compared to that of methods requiring semiglobal potential surfaces or variational treatments of the rovibronic Hamiltonian. Such applications include spectral characterization of comets, exoplanets, or any situation in which gas phase molecules are being excited by UV-vis radiation.
Collapse
Affiliation(s)
- Noah R Garrett
- Department of Chemistry & Biochemistry, University of Mississippi, University, Mississippi 38677-1848, United States
| | - Megan C Davis
- Theoretical Division, T-1, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, United States
- Center for Nonlinear Studies, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, United States
| | - Ryan C Fortenberry
- Department of Chemistry & Biochemistry, University of Mississippi, University, Mississippi 38677-1848, United States
| |
Collapse
|
5
|
Gudipati MS, Fleury B, Wagner R, Henderson BL, Altwegg K, Rubin M. Thermal behavior of astrophysical amorphous molecular ices. Faraday Discuss 2023; 245:467-487. [PMID: 37341061 DOI: 10.1039/d3fd00048f] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 06/22/2023]
Abstract
Ice is a major component of astrophysical environments - from interstellar molecular clouds through protoplanetary disks to evolved solar systems. Ice and complex organic matter coexist in these environments as well, and it is thought primordial ice brought the molecules of life to Earth four billion years ago, which could have kickstarted the origin of life on Earth. To understand the journey of ice and organics from their origins to becoming a part of evolved planetary systems, it is important to complement high spatial and spectral resolution telescopes such as JWST with laboratory experimental studies that provide deeper insight into the processes that occur in these astrophysical environments. Our laboratory studies are aimed at providing this knowledge. In this article we present simultaneous mass spectrometric and infrared spectroscopic investigation on how molecular ice mixtures behave at different temperatures and how this information is critical to interpret observational data from protoplanetary disks as well as comets. We find that amorphous to crystalline water ice transformation is the most critical phenomenon that differentiates between outgassing of trapped volatiles such as CO2vs. outgassing of pure molecular ice domains of the same in a mixed molecular ice. Crystalline water ice is found to trap only a small fraction of other volatiles (<5%), indicating ice grain composition in astrophysical and planetary environments must be different depending on whether the ice is in amorphous phase or transformed into crystalline phase, even if the crystalline ice undergoes radiation-induced amorphization subsequently. Crystallization of water ice is a key differentiator for many ices in astronomical environments as well as in our Solar System.
Collapse
Affiliation(s)
- Murthy S Gudipati
- Science Division, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
| | - Benjamin Fleury
- Univ Paris Est Creteil and Université Paris Cité, CNRS, LISA, F-94010 Créteil, France
| | - Robert Wagner
- Institute of Meteorology and Climate Research, Karlsruhe Institute of Technology, Karlsruhe, Germany
| | - Bryana L Henderson
- Science Division, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
| | - Kathrin Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| |
Collapse
|
6
|
Chang Y, Ashfold MNR, Yuan K, Yang X. Exploring the vacuum ultraviolet photochemistry of astrochemically important triatomic molecules. Natl Sci Rev 2023; 10:nwad158. [PMID: 37771464 PMCID: PMC10533343 DOI: 10.1093/nsr/nwad158] [Citation(s) in RCA: 6] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/19/2022] [Revised: 11/03/2022] [Accepted: 02/08/2023] [Indexed: 09/30/2023] Open
Abstract
The recently constructed vacuum ultraviolet (VUV) free electron laser (FEL) at the Dalian Coherent Light Source (DCLS) is yielding a wealth of new and exquisitely detailed information about the photofragmentation dynamics of many small gas-phase molecules. This Review focuses particular attention on five triatomic molecules-H2O, H2S, CO2, OCS and CS2. Each shows excitation wavelength-dependent dissociation dynamics, yielding photofragments that populate a range of electronic and (in the case of diatomic fragments) vibrational and rotational quantum states, which can be characterized by different translational spectroscopy methods. The photodissociation of an isolated molecule from a well-defined initial quantum state provides a lens through which one can investigate how and why chemical reactions occur, and provides numerous opportunities for fruitful, synergistic collaborations with high-level ab initio quantum chemists. The chosen molecules, their photofragments and the subsequent chemical reaction networks to which they can contribute are all crucial in planetary atmospheres and in interstellar and circumstellar environments. The aims of this Review are 3-fold: to highlight new photochemical insights enabled by the VUV-FEL at the DCLS, notably the recently recognized central atom elimination process that is shown to contribute in all of these triatomic molecules; to highlight some of the potential implications of this rich photochemistry to our understanding of interstellar chemistry and molecular evolution within the universe; and to highlight other and future research directions in areas related to chemical reaction dynamics and astrochemistry that will be enabled by increased access to VUV-FEL sources.
Collapse
Affiliation(s)
- Yao Chang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian 116023, China
| | | | - Kaijun Yuan
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian 116023, China
- University of Chinese Academy of Sciences, Beijing 100049, China
- Hefei National Laboratory, Hefei 230088, China
| | - Xueming Yang
- State Key Laboratory of Molecular Reaction Dynamics and Dalian Coherent Light Source, Dalian Institute of Chemical Physics, Chinese Academy of Sciences, Dalian 116023, China
- Hefei National Laboratory, Hefei 230088, China
- Department of Chemistry, College of Science, Southern University of Science and Technology, Shenzhen 518055, China
| |
Collapse
|
7
|
Harwick OA, Fortenberry RC. Spectroscopic Constants and Anharmonic Vibrational Frequencies of C(O)OC, c-C 2O 2 and Their Silicon-Containing Analogues. Molecules 2023; 28:molecules28114563. [PMID: 37299037 DOI: 10.3390/molecules28114563] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/11/2023] [Revised: 05/31/2023] [Accepted: 06/01/2023] [Indexed: 06/12/2023] Open
Abstract
Comets are likely to contain various carbon oxide molecules potentially including C(O)OC and c-C2O2 on their surfaces and comae, as well as their silicon-substituted analogues possibly playing a role in the formation of interstellar dust grains. In this work, high-level quantum chemical data are provided to support such potential future astrophysical detection through the generation of predicted rovibrational data. Laboratory-based chemistry would also benefit from such aforementioned computational benchmarking considering these molecules' historic computational and experimental elusiveness. Coupled-cluster singles, doubles, and perturbative triples, the F12b formalism, and the cc-pCVTZ-F12 basis set garner the rapid, yet highly trusted F12-TcCR level of theory leveraged presently. This current work points to all four molecules' strong IR activity, coupled with large intensities, thus suggesting the potential for JWST detection. Although Si(O)OSi possesses a permanent dipole moment significantly larger than those of the other molecules of present interest, the significant abundance of the potential precursor carbon monoxide suggests that the dicarbon dioxide molecules may yet be observable in the microwave region of the electromagnetic spectrum. Thus, this present work details the likely existence and detectability of these four cyclic molecules, providing updated implications compared to previous work performed both experimentally and computationally.
Collapse
Affiliation(s)
- Olivia A Harwick
- Department of Chemistry and Biochemistry, University of Mississippi, University, MS 38677, USA
| | - Ryan C Fortenberry
- Department of Chemistry and Biochemistry, University of Mississippi, University, MS 38677, USA
| |
Collapse
|
8
|
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.
Collapse
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
| |
Collapse
|
9
|
He C, Luo Y, Doddipatla S, Yang Z, Millar TJ, Sun R, Kaiser RI. Gas-phase formation of silicon monoxide via non-adiabatic reaction dynamics and its role as a building block of interstellar silicates. Phys Chem Chem Phys 2022; 24:19761-19772. [PMID: 35971984 DOI: 10.1039/d2cp02188a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
Silicon monoxide (SiO) is classified as a key precursor and fundamental molecular building block to interstellar silicate nanoparticles, which play an essential role in the synthesis of molecular building blocks connected to the Origins of Life. In the cold interstellar medium, silicon monoxide is of critical importance in initiating a series of elementary chemical reactions leading to larger silicon oxides and eventually to silicates. To date, the fundamental formation mechanisms and chemical dynamics leading to gas phase silicon monoxide have remained largely elusive. Here, through a concerted effort between crossed molecular beam experiments and electronic structure calculations, it is revealed that instead of forming highly-stable silicon dioxide (SiO2), silicon monoxide can be formed via a barrierless, exoergic, single-collision event between ground state molecular oxygen and atomic silicon involving non-adiabatic reaction dynamics through various intersystem crossings. Our research affords persuasive evidence for a likely source of highly rovibrationally excited silicon monoxide in cold molecular clouds thus initiating the complex chain of exoergic reactions leading ultimately to a population of silicates at low temperatures in our Galaxy.
Collapse
Affiliation(s)
- Chao He
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Yuheng Luo
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Srinivas Doddipatla
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Zhenghai Yang
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Tom J Millar
- School of Mathematics and Physics, Queen's University Belfast, University Road, Belfast, BT7 1NN, UK
| | - Rui Sun
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI 96822, USA.
| |
Collapse
|
10
|
Mifsud DV, Kaňuchová Z, Ioppolo S, Herczku P, Traspas Muiña A, Sulik B, Rahul KK, Kovács STS, Hailey PA, McCullough RW, Mason NJ, Juhász Z. Ozone production in electron irradiated CO 2:O 2 ices. Phys Chem Chem Phys 2022; 24:18169-18178. [PMID: 35861183 DOI: 10.1039/d2cp01535h] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
The detection of ozone (O3) in the surface ices of Ganymede, Jupiter's largest moon, and of the Saturnian moons Rhea and Dione, has motivated several studies on the route of formation of this species. Previous studies have successfully quantified trends in the production of O3 as a result of the irradiation of pure molecular ices using ultraviolet photons and charged particles (i.e., ions and electrons), such as the abundances of O3 formed after irradiation at different temperatures or using different charged particles. In this study, we extend such results by quantifying the abundance of O3 as a result of the 1 keV electron irradiation of a series of 14 stoichiometrically distinct CO2:O2 astrophysical ice analogues at 20 K. By using mid-infrared spectroscopy as our primary analytical tool, we have also been able to perform a spectral analysis of the asymmetric stretching mode of solid O3 and the variation in its observed shape and profile among the investigated ice mixtures. Our results are important in the context of better understanding the surface composition and chemistry of icy outer Solar System objects, and may thus be of use to future interplanetary space missions such as the ESA Jupiter Icy Moons Explorer and the NASA Europa Clipper missions, as well as the recently launched NASA James Webb Space Telescope.
Collapse
Affiliation(s)
- Duncan V Mifsud
- Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury CT2 7NH, UK. .,Institute for Nuclear Research (Atomki), Debrecen H-4026, Hungary.
| | - Zuzana Kaňuchová
- Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica SK-059 60, Slovakia.
| | - Sergio Ioppolo
- School of Electronic Engineering and Computer Science, Queen Mary University of London, London E1 4NS, UK.
| | - Péter Herczku
- Institute for Nuclear Research (Atomki), Debrecen H-4026, Hungary.
| | - Alejandra Traspas Muiña
- School of Electronic Engineering and Computer Science, Queen Mary University of London, London E1 4NS, UK.
| | - Béla Sulik
- Institute for Nuclear Research (Atomki), Debrecen H-4026, Hungary.
| | - K K Rahul
- Institute for Nuclear Research (Atomki), Debrecen H-4026, Hungary.
| | | | - Perry A Hailey
- Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury CT2 7NH, UK.
| | - Robert W McCullough
- Department of Physics and Astronomy, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK
| | - Nigel J Mason
- Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury CT2 7NH, UK.
| | - Zoltán Juhász
- Institute for Nuclear Research (Atomki), Debrecen H-4026, Hungary.
| |
Collapse
|
11
|
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.
Collapse
|
12
|
An S, Ranjan S, Yuan K, Yang X, Skodje RT. The role of the three body photodissociation channel of water in the evolution of dioxygen in astrophysical applications. Phys Chem Chem Phys 2021; 23:9235-9248. [PMID: 33885109 DOI: 10.1039/d1cp00565k] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
A recent experiment at the Dalian Coherent Light Source (DCLS) has provided measurements of the partial cross sections for the photodissociation of water vapor over an unprecedented range of wavelengths in the vacuum ultraviolet (VUV) region. It was found that the three body dissociation channel, H + H + O(3P/1D), becomes prominent at wavelengths shorter than the Lyman α-line at 121.6 nm. The present work explores the kinetic consequences of this discovery for several astrophysically motivated examples. The irradiation of a dilute low-temperature gas by unscreened solar radiation, similar to early stage photochemical processing in a comet coma, shows significant increase in the production of O2-molecules at shorter times, <1 day, that might physically correspond to the photochemical reaction zone of the coma. Several examples of planetary atmospheres show increased O-atom production at high altitudes but relatively little modification of the equilibrium O2 concentrations predicted by conventional models.
Collapse
Affiliation(s)
- Suming An
- Department of Chemistry, University of Colorado, Boulder, CO 80309-215, USA.
| | | | | | | | | |
Collapse
|
13
|
Ferrari BC, Slavicinska K, Bennett CJ. Role of Suprathermal Chemistry on the Evolution of Carbon Oxides and Organics within Interstellar and Cometary Ices. Acc Chem Res 2021; 54:1067-1079. [PMID: 33554606 DOI: 10.1021/acs.accounts.0c00731] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/29/2022]
Abstract
ConspectusLaboratory-based experimental astrochemistry regularly entails simulation of astrophysical environments whereby low-temperature condensed ices are exposed to radiation from ultraviolet (UV) photons or energetic charged particles. Here, excited atoms/radicals are generated that are not in thermal equilibrium with their surroundings (i.e., they are nonthermal, or suprathermal). These species can surpass typical reaction barriers and partake in unusual chemical processes leading to novel molecular species. Often, these are uniquely observable under low-temperature conditions where the surrounding ice matrix can stabilize excited intermediates that would otherwise fall apart. Fourier-transform infrared (FTIR) spectroscopy is traditionally utilized to monitor the evolution of chemical species within ices in situ during radiolysis. Yet, the characterization and quantification of novel species and radicals formed within astrophysical ices is often hindered since many of these cannot be synthesized by traditional synthetic chemistry. Computational approaches can provide fundamental vibrational frequencies and isotopic shifts to help aid in assignments alongside infrared intensities and Raman activities to quantify levels of production. In this Account, we begin with a brief history and background regarding the composition and radiation of interstellar ices. We review details of some of the early work on carbon oxides produced during the radiolysis of pure carbon dioxide ices and contention around the carrier of an absorption feature that could potentially be a product of radiation. We then provide an overview of current and emerging experimental methodologies and some of the chemistries that occur via nonthermal processes during radiolysis of low-temperature ices. Next, we detail computational approaches to reliably predict vibrational frequencies, infrared intensities, and Raman activities based on our recent work. Our focus then turns to studies on the formation of complex organics and carbon oxides, highlighting those aided by computational approaches and their role in astrochemistry. Some recent controversies regarding assignments alongside our recent results on the characterization of novel carbon oxide species are discussed. We present an argument for the potential role of carbon oxides within cometary ices as parent molecular species for small volatiles. We provide an overview of some of the complex organic species that can be formed within interstellar and cometary ices that contain either carbon monoxide or carbon dioxide. We examine how Raman spectroscopy could potentially be leveraged to help determine and characterize carbon oxides in future experiments as well as how computational approaches can aid in these assignments. We conclude with brief remarks on future directions our research group is taking to unravel astrochemically relevant carbon oxides using combined computational and experimental approaches.
Collapse
Affiliation(s)
- Brian C. Ferrari
- Department of Physics, University of Central Florida, Orlando, Florida 32816, United States
| | - Katerina Slavicinska
- Department of Physics, University of Central Florida, Orlando, Florida 32816, United States
| | - Christopher J. Bennett
- Department of Physics, University of Central Florida, Orlando, Florida 32816, United States
| |
Collapse
|
14
|
McKay AJ, Roth NX. Organic Matter in Cometary Environments. Life (Basel) 2021; 11:37. [PMID: 33430031 PMCID: PMC7826631 DOI: 10.3390/life11010037] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/07/2020] [Revised: 12/28/2020] [Accepted: 01/01/2021] [Indexed: 11/16/2022] Open
Abstract
Comets contain primitive material leftover from the formation of the Solar System, making studies of their composition important for understanding the formation of volatile material in the early Solar System. This includes organic molecules, which, for the purpose of this review, we define as compounds with C-H and/or C-C bonds. In this review, we discuss the history and recent breakthroughs of the study of organic matter in comets, from simple organic molecules and photodissociation fragments to large macromolecular structures. We summarize results both from Earth-based studies as well as spacecraft missions to comets, highlighted by the Rosetta mission, which orbited comet 67P/Churyumov-Gerasimenko for two years, providing unprecedented insights into the nature of comets. We conclude with future prospects for the study of organic matter in comets.
Collapse
Affiliation(s)
- Adam J. McKay
- Department of Physics, American University, Washington, DC 20016, USA
- Planetary Systems Laboratory Code 693, Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Nathan X. Roth
- Astrochemistry Laboratory Code 691, Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA;
- Universities Space Research Association, Columbia, MD 21046, USA
| |
Collapse
|
15
|
Ferrari BC, Bennett CJ. A computational investigation of the equilibrium geometries, energetics, vibrational frequencies, infrared intensities and Raman activities of C2Oy (y = 3, 4) species. Mol Phys 2020. [DOI: 10.1080/00268976.2020.1837404] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/23/2022]
Affiliation(s)
- Brian C. Ferrari
- Department of Physics, University of Central Florida, Orlando, FL, USA
| | - Chris J. Bennett
- Department of Physics, University of Central Florida, Orlando, FL, USA
| |
Collapse
|
16
|
Cometary panspermia and origin of life? ADVANCES IN GENETICS 2020. [PMID: 33081926 DOI: 10.1016/bs.adgen.2020.03.003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register]
Abstract
A range of astronomical observations are shown to be in accord with the theory of cometary panspermia. This theory posits that comets harbor a viable biological component in the form of bacteria and viruses that led to origin and evolution of life on Earth. The data includes (1) infrared, visual and ultraviolet spectra of interstellar dust, (2) infrared spectra of the dust released from comet Halley in 1986, (3) infrared spectra of comet Hale-Bopp in 1997, (4) near and mid-infrared spectra of comet Tempel I in 2005, (5) the discovery of an amino acid and degradation products attributable to biology in the material recovered from the Stardust Mission in 2009, (6) jets from comet Lovejoy showing both a sugar and Ethyl alcohol and finally, (7) a diverse set of data that has emerged from the Rosetta mission. The conjunction of all the available data points to cometary biology and interstellar panspermia as being inevitable.
Collapse
|
17
|
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.
Collapse
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
| |
Collapse
|
18
|
Qasim D, Witlox MJA, Fedoseev G, Chuang KJ, Banu T, Krasnokutski SA, Ioppolo S, Kästner J, van Dishoeck EF, Linnartz H. A cryogenic ice setup to simulate carbon atom reactions in interstellar ices. THE REVIEW OF SCIENTIFIC INSTRUMENTS 2020; 91:054501. [PMID: 32486761 DOI: 10.1063/5.0003692] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/04/2020] [Accepted: 04/14/2020] [Indexed: 06/11/2023]
Abstract
The design, implementation, and performance of a customized carbon atom beam source for the purpose of investigating solid-state reaction routes in interstellar ices in molecular clouds are discussed. The source is integrated into an existing ultrahigh vacuum setup, SURFace REaction SImulation DEvice (SURFRESIDE2), which extends this double atom (H/D, O, and N) beamline apparatus with a third atom (C) beamline to a unique system that is fully suited to explore complex organic molecule solid-state formation under representative interstellar cloud conditions. The parameter space for this system is discussed, which includes the flux of the carbon atoms hitting the ice sample, their temperature, and the potential impact of temperature on ice reactions. Much effort has been put into constraining the beam size to within the limits of the sample size with the aim of reducing carbon pollution inside the setup. How the C-atom beam performs is quantitatively studied through the example experiment, C + 18O2, and supported by computationally derived activation barriers. The potential for this source to study the solid-state formation of interstellar complex organic molecules through C-atom reactions is discussed.
Collapse
Affiliation(s)
- D Qasim
- Laboratory for Astrophysics, Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands
| | - M J A Witlox
- Fine Mechanical Department, Leiden Institute for Physics Research (LION), Niels Bohrweg 2, NL-2333 CA Leiden, The Netherlands
| | - G Fedoseev
- Laboratory for Astrophysics, Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands
| | - K-J Chuang
- Laboratory Astrophysics Group of the Max Planck Institute for Astronomy at the Friedrich Schiller University Jena, Institute of Solid State Physics, Helmholtzweg 3, D-07743 Jena, Germany
| | - T Banu
- Institute for Theoretical Chemistry, University of Stuttgart, D-70569 Stuttgart, Germany
| | - S A Krasnokutski
- Laboratory Astrophysics Group of the Max Planck Institute for Astronomy at the Friedrich Schiller University Jena, Institute of Solid State Physics, Helmholtzweg 3, D-07743 Jena, Germany
| | - S Ioppolo
- School of Electronic Engineering and Computer Science, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
| | - J Kästner
- Institute for Theoretical Chemistry, University of Stuttgart, D-70569 Stuttgart, Germany
| | - E F van Dishoeck
- Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands
| | - H Linnartz
- Laboratory for Astrophysics, Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands
| |
Collapse
|
19
|
Bekaert DV, Broadley MW, Marty B. The origin and fate of volatile elements on Earth revisited in light of noble gas data obtained from comet 67P/Churyumov-Gerasimenko. Sci Rep 2020; 10:5796. [PMID: 32242104 PMCID: PMC7118078 DOI: 10.1038/s41598-020-62650-3] [Citation(s) in RCA: 15] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/03/2019] [Accepted: 03/17/2020] [Indexed: 11/25/2022] Open
Abstract
The origin of terrestrial volatiles remains one of the most puzzling questions in planetary sciences. The timing and composition of chondritic and cometary deliveries to Earth has remained enigmatic due to the paucity of reliable measurements of cometary material. This work uses recently measured volatile elemental ratios and noble gas isotope data from comet 67P/Churyumov-Gerasimenko (67P/C-G), in combination with chondritic data from the literature, to reconstruct the composition of Earth’s ancient atmosphere. Comets are found to have contributed ~20% of atmospheric heavy noble gases (i.e., Kr and Xe) but limited amounts of other volatile elements (water, halogens and likely organic materials) to Earth. These cometary noble gases were likely mixed with chondritic - and not solar - sources to form the atmosphere. We show that an ancient atmosphere composed of chondritic and cometary volatiles is more enriched in Xe relative to the modern atmosphere, requiring that 8–12 times the present-day inventory of Xe was lost to space. This potentially resolves the long-standing mystery of Earth’s “missing xenon”, with regards to both Xe elemental depletion and isotopic fractionation in the atmosphere. The inferred Kr/H2O and Xe/H2O of the initial atmosphere suggest that Earth’s surface volatiles might not have been fully delivered by the late accretion of volatile-rich carbonaceous chondrites. Instead, “dry” materials akin to enstatite chondrites potentially constituted a significant source of chondritic volatiles now residing on the Earth’s surface. We outline the working hypotheses, implications and limitations of this model in the last section of this contribution.
Collapse
Affiliation(s)
- David V Bekaert
- Centre de Recherches Pétrographiques et Géochimiques, UMR 7358 CNRS - Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501, Vandoeuvre-lès-Nancy, France.
| | - Michael W Broadley
- Centre de Recherches Pétrographiques et Géochimiques, UMR 7358 CNRS - Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501, Vandoeuvre-lès-Nancy, France.
| | - Bernard Marty
- Centre de Recherches Pétrographiques et Géochimiques, UMR 7358 CNRS - Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501, Vandoeuvre-lès-Nancy, France
| |
Collapse
|
20
|
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.
Collapse
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
| |
Collapse
|
21
|
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.
Collapse
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
| |
Collapse
|
22
|
Rovibrational Spectral Analysis of CO3 and C2O3: Potential Sources for O2 Observed in Comet 67P/Churyumov–Gerasimenko. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab53e8] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/20/2022]
|
23
|
Kim SY, Lee JY, Jhin C, Shin JM, Kim M, Ahn HR, Yoo G, Son YJ, Jung SH, Nho CW. Reduction of Hepatic Lipogenesis by Loliolide and Pinoresinol from Lysimachia vulgaris via Degrading Liver X Receptors. JOURNAL OF AGRICULTURAL AND FOOD CHEMISTRY 2019; 67:12419-12427. [PMID: 31610126 DOI: 10.1021/acs.jafc.9b01488] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
The liver X receptors (LXRs) are major regulators of lipogenesis, and their reduced activation by an inhibitor could be a treatment strategy for fatty liver disease. Small molecules originating from dietary food are considered suitable and attractive drug candidates for humans in terms of safety. In this study, an edible plant, Lysimachia vulgaris (LV), used as a traditional and medicinal food in East Asia was evaluated for lipogenesis decreasing effects. Activity-guided fractionation was performed, and the isolated compounds were identified using spectroscopic methods. We conducted in vitro real-time polymerase chain reaction (PCR) and Western blotting as well as histological and biochemical analyses following in vivo treatments. Using a high-fat diet animal model, we confirmed that LV extracts (LVE) decreased lipogenic metabolism and restored liver function to control levels. To identify active components, we conducted activity-guided fractionation and then isolated compounds. Two compounds, loliolide and pinoresinol, were identified in the dichloromethane fraction, and they significantly attenuated the expression levels of lipogenic factors including sterol regulatory element-binding protein (SREBP)-1, stearoyl-CoA desaturase 1 (SCD1), fatty acid synthase (FAS), and acetyl-CoA carboxylase (ACC). Importantly, loliolide and pinoresinol significantly accelerated the protein degradation of LXRs by enhanced ubiquitination, which inhibited lipogenesis. These results suggest that loliolide and pinoresinol might be potential candidate supplementary treatments for nonalcoholic fatty liver disease (NAFLD) by reducing lipogenesis through increased ubiquitination of LXRs.
Collapse
Affiliation(s)
- Sun Young Kim
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Joo Young Lee
- Natural Products Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Changho Jhin
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Ji Min Shin
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
- Department of Biological Chemistry , University of Science and Technology (UST) , Daejeon 34113 , Republic of Korea
| | - Myungsuk Kim
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Hong Ruyl Ahn
- Natural Products Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Gyhye Yoo
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Yang-Ju Son
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Sang Hoon Jung
- Natural Products Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| | - Chu Won Nho
- Smart Farm Research Center , Korea Institute of Science and Technology (KIST) , Gangneung 25451 , Republic of Korea
| |
Collapse
|
24
|
Garrod RT. Simulations of ice chemistry in cometary nuclei. THE ASTROPHYSICAL JOURNAL 2019; 884:10.3847/1538-4357/ab418e. [PMID: 31806913 PMCID: PMC6894404 DOI: 10.3847/1538-4357/ab418e] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
The first computational model of solid-phase chemistry in cometary nuclear ices is presented. An astrochemical kinetics model, MAGICKAL, is adapted to trace the chemical evolution in multiple layers of cometary ice, over a representative period of 5 Gyr. Physical conditions are chosen appropriate for "cold storage" of the cometary nucleus in the outer Solar System, prior to any active phase. The chemistry is simulated at a selection of static temperatures in the range 5 - 60 K, while the ice is exposed to the interstellar radiation field, inducing a photo-chemistry in the outer ice layers that produces significant formation of complex organic molecules. A treatment for the chemistry resulting from cosmic-ray bombardment of the ices is also introduced into the model, along with a new formulation for low-temperature photo-chemistry. Production of simple and complex molecules to depth on the order of 10 m or more is achieved, with local fractional abundances comparable to observed values in many cases. The production of substantial amounts of O2 (and H2O2) is found, suggesting that long-term processing by high-energy cosmic rays of cometary ices in situ, over a period on the order of 1 Gyr, may be sufficient to explain the large observed abundances of O2, if the overall loss of material from the comet is limited to a depth on the order of 10 m. Entry into the inner solar system could produce a further enhancement in the molecular content of the nuclear ices that may be quantifiable using this modeling approach.
Collapse
Affiliation(s)
- Robin T Garrod
- Departments of Astronomy and Chemistry, University of Virginia, Charlottesville, VA 22904
| |
Collapse
|
25
|
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.
Collapse
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
| |
Collapse
|
26
|
Cunsolo V, Foti S, Ner‐Kluza J, Drabik A, Silberring J, Muccilli V, Saletti R, Pawlak K, Harwood E, Yu F, Ciborowski P, Anczkiewicz R, Altweg K, Spoto G, Pawlaczyk A, Szynkowska MI, Smoluch M, Kwiatkowska D. Mass Spectrometry Applications. Mass Spectrom (Tokyo) 2019. [DOI: 10.1002/9781119377368.ch8] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022] Open
|
27
|
The Effective Surface Area of Amorphous Solid Water Measured by the Infrared Absorption of Carbon Monoxide. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab1f6a] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
|
28
|
Fortenberry RC, Trabelsi T, Westbrook BR, Del Rio WA, Francisco JS. Molecular oxygen generation from the reaction of water cations with oxygen atoms. J Chem Phys 2019; 150:201103. [PMID: 31153175 DOI: 10.1063/1.5102073] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The oxywater cation (H2OO+), previously shown to form barrierlessly in the gas phase from water cations and atomic oxygen, is proposed here potentially to possess a 2A″ ←4A″ excitation leading to the H2⋯O2 + complex. This complex could then easily decompose into molecular hydrogen and the molecular oxygen cation. The present quantum chemical study shows that the necessary electronic transition takes place in the range of 1.92 eV (645 nm), in the orange-red range of the visible and solar spectrum, and dissociation of the complex only requires 5.8 kcal/mol (0.25 eV). Such a process for the abiotic, gas phase formation of O2 would only need to be photocatalyzed by visible wavelength photons. Hence, such a process could produce O2 at the mesosphere/stratosphere boundary as climate change is driving more water into the upper atmosphere, in the comet 67P/Churyumov-Gerasimenko where surprisingly high levels of O2 have been observed, or at gas-surface (ice) interfaces.
Collapse
Affiliation(s)
- Ryan C Fortenberry
- Department of Chemistry and Biochemistry, University of Mississippi, University, Mississippi 38677-1848, USA
| | - Tarek Trabelsi
- Department of Earth and Environmental Science Philadelphia, University of Pennsylvania, Philadelphia, Pennsylvania 19104, USA
| | - Brent R Westbrook
- Department of Chemistry, St. Edward's University, Austin, Texas 78704, USA
| | - Weston A Del Rio
- Department of Chemistry and Biochemistry, University of Mississippi, University, Mississippi 38677-1848, USA
| | - Joseph S Francisco
- Department of Earth and Environmental Science Philadelphia, University of Pennsylvania, Philadelphia, Pennsylvania 19104, USA
| |
Collapse
|
29
|
Direct dioxygen evolution in collisions of carbon dioxide with surfaces. Nat Commun 2019; 10:2294. [PMID: 31127109 PMCID: PMC6534623 DOI: 10.1038/s41467-019-10342-6] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/09/2018] [Accepted: 04/29/2019] [Indexed: 11/18/2022] Open
Abstract
The intramolecular conversion of CO2 to molecular oxygen is an exotic reaction, rarely observed even with extreme optical or electronic excitation means. Here we show that this reaction occurs readily when CO2 ions scatter from solid surfaces in a two-step sequential collision process at hyperthermal incidence energies. The produced O2 is preferentially ionized by charge transfer from the surface over the predominant atomic oxygen product, leading to direct detection of both O2+ and O2−. First-principles simulations of the collisional dynamics reveal that O2 production proceeds via strongly-bent CO2 configurations, without visiting other intermediates. Bent CO2 provides dynamic access to the symmetric dissociation of CO2 to C+O2 with a calculated yield of 1 to 2% depending on molecular orientation. This unexpected collision-induced transformation of individual CO2 molecules provides an accessible pathway for generating O2 in astrophysical environments and may inspire plasma-driven electro- and photo-catalytic strategies for terrestrial CO2 reduction. Carbon dioxide can dissociate via different pathways depending on the amount of available energy. Here the authors investigate carbon dioxide collisions with metal substrates and observe a pathway producing molecular oxygen, which might explain the presence of oxygen in abiotic environments.
Collapse
|
30
|
Stellar Occultation by Comet 67P/Churyumov–Gerasimenko Observed with Rosetta's Alice Far-ultraviolet Spectrograph. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-3881/ab1097] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
|
31
|
Liu YW, Peng YG, Xiong T, Wang SX, Huang XC, Wu Y, Zhu LF. Generalized oscillator strengths of the low-lying valence-shell excitations of N 2, O 2, and C 2H 2 studied by fast electron and inelastic x-ray scattering. J Chem Phys 2019; 150:094302. [PMID: 30849870 DOI: 10.1063/1.5087603] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
Abstract
The generalized oscillator strengths of the low-lying valence-shell excitations of N2, O2, and C2H2 have been studied by the high-energy electron scattering, the high-resolution inelastic X-ray scattering, and the multireference single- and double-excitation configuration-interaction methods. Good agreement between the present electron-scattering results and the X-ray-scattering ones for the a''1Σg +v'=0 and a''1Σg +v'=1+b1Πuv'=0 excitations of N2 and the A'3Δu excitation of O2 is achieved in the small squared momentum transfer region, while obvious discrepancies among them are observed in the large squared momentum transfer region. This phenomenon indicates that the first Born approximation is satisfied in the small squared momentum transfer region, while it does not hold in the large squared momentum transfer region at an incident electron energy of 1500 eV, in view of the fact that the first Born approximation is satisfied in the X-ray scattering. In addition, the present calculation for the a''1Σg + excitation shows that the traditional assigned v' = 0 and 1 of the a″1Σg + excitation correspond to v' = 9 and 13 of the 21Σg + excitation and reproduces the X-ray-scattering results of the a''1Σg +v'=0 excitation very well except the ones in the small squared momentum transfer region. We also report the generalized oscillator strengths of the à + B̃ excitations of C2H2, and its profile shows that the bending geometry has great influence on the transition feature.
Collapse
Affiliation(s)
- Ya-Wei Liu
- Hefei National Laboratory for Physical Sciences at Microscale and Department of Modern Physics, University of Science and Technology of China, Hefei, Anhui 230026, People's Republic of China
| | - Yi-Geng Peng
- Data Center for High Energy Density Physics, Institute of Applied Physics and Computational Mathematics, P.O. Box 8009, Beijing 100088, People's Republic of China
| | - Tao Xiong
- Hefei National Laboratory for Physical Sciences at Microscale and Department of Modern Physics, University of Science and Technology of China, Hefei, Anhui 230026, People's Republic of China
| | - Shu-Xing Wang
- Hefei National Laboratory for Physical Sciences at Microscale and Department of Modern Physics, University of Science and Technology of China, Hefei, Anhui 230026, People's Republic of China
| | - Xin-Chao Huang
- Hefei National Laboratory for Physical Sciences at Microscale and Department of Modern Physics, University of Science and Technology of China, Hefei, Anhui 230026, People's Republic of China
| | - Yong Wu
- Data Center for High Energy Density Physics, Institute of Applied Physics and Computational Mathematics, P.O. Box 8009, Beijing 100088, People's Republic of China
| | - Lin-Fan Zhu
- Hefei National Laboratory for Physical Sciences at Microscale and Department of Modern Physics, University of Science and Technology of China, Hefei, Anhui 230026, People's Republic of China
| |
Collapse
|
32
|
Fortenberry RC, Lee TJ. Computational vibrational spectroscopy for the detection of molecules in space. ANNUAL REPORTS IN COMPUTATIONAL CHEMISTRY 2019. [DOI: 10.1016/bs.arcc.2019.08.006] [Citation(s) in RCA: 36] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/28/2023]
|
33
|
Luspay-Kuti A, Mousis O, Lunine JI, Ellinger Y, Pauzat F, Raut U, Bouquet A, Mandt KE, Maggiolo R, Ronnet T, Brugger B, Ozgurel O, Fuselier SA. Origin of Molecular Oxygen in Comets: Current Knowledge and Perspectives. SPACE SCIENCE REVIEWS 2018; 214:115. [PMID: 30613113 PMCID: PMC6317742 DOI: 10.1007/s11214-018-0541-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [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) instrument onboard the Rosetta spacecraft has measured molecular oxygen (O2) in the coma of comet 67P/Churyumov-Gerasimenko (67P/C-G) in surprisingly high abundances. These measurements mark the first unequivocal detection of O2 in a cometary environment. The large relative abundance of O2 in 67P/C-G despite its high reactivity and low interstellar abundance poses a puzzle for its origin in comet 67P/C-G, and potentially other comets. Since its detection, there have been a number of hypotheses put forward to explain the production and origin of O2 in the comet. These hypotheses cover a wide range of possibilities from various in situ production mechanisms to protosolar nebula and primordial origins. Here, we review the O2 formation mechanisms from the literature, and provide a comprehensive summary of the current state of knowledge of the sources and origin of cometary O2.
Collapse
Affiliation(s)
- Adrienn Luspay-Kuti
- Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA
| | - Olivier Mousis
- Laboratoire d'Astrophysique de Marseille, UMR CNRS 7326, Aix-Marseille Université & OSU Pythéas, Marseille, France
| | - Jonathan I Lunine
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853, USA
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - Yves Ellinger
- CNRS, Laboratoire de Chimie Théorique, LCT, Sorbonne Université, 75005 Paris, France
| | - Françoise Pauzat
- CNRS, Laboratoire de Chimie Théorique, LCT, Sorbonne Université, 75005 Paris, France
| | - Ujjwal Raut
- Department of Space Research, Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX 78238, USA
| | - Alexis Bouquet
- Department of Space Research, Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX 78238, USA
- Department of Physics and Astronomy, University of Texas at San Antonio, One UTSA Circle, San Antonio, TX 78249, USA
| | - Kathleen E Mandt
- Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA
| | - Romain Maggiolo
- Royal Institute for Space Aeronomy, 3 Avenue Circulaire, Brussels, Belgium
| | - Thomas Ronnet
- Laboratoire d'Astrophysique de Marseille, UMR CNRS 7326, Aix-Marseille Université & OSU Pythéas, Marseille, France
| | - Bastien Brugger
- Laboratoire d'Astrophysique de Marseille, UMR CNRS 7326, Aix-Marseille Université & OSU Pythéas, Marseille, France
| | - Ozge Ozgurel
- CNRS, Laboratoire de Chimie Théorique, LCT, Sorbonne Université, 75005 Paris, France
| | - Stephen A Fuselier
- Department of Space Research, Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX 78238, USA
- Department of Physics and Astronomy, University of Texas at San Antonio, One UTSA Circle, San Antonio, TX 78249, USA
| |
Collapse
|
34
|
Bishwakarma CK, van Oevelen G, Scheidsbach R, Parker DH, Kalugina Y, Lique F. Communication: State-to-state inelastic scattering of interstellar O 2 with H 2. J Chem Phys 2018; 149:121101. [DOI: 10.1063/1.5051610] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Affiliation(s)
- Chandan Kumar Bishwakarma
- Institute for Molecules and Materials, Radboud University Nijmegen, Heijendaalseweg 135, 6525 AJ Nijmegen, The Netherlands
| | - George van Oevelen
- Institute for Molecules and Materials, Radboud University Nijmegen, Heijendaalseweg 135, 6525 AJ Nijmegen, The Netherlands
| | - Roy Scheidsbach
- Institute for Molecules and Materials, Radboud University Nijmegen, Heijendaalseweg 135, 6525 AJ Nijmegen, The Netherlands
| | - David H. Parker
- Institute for Molecules and Materials, Radboud University Nijmegen, Heijendaalseweg 135, 6525 AJ Nijmegen, The Netherlands
| | - Yulia Kalugina
- Tomsk State University, Ave. Lenin, 36, 634050 Tomsk, Russia and Institute of Spectroscopy, Russian Academy of Sciences, Fizicheskaya St. 5, 108840 Troitsk, Moscow, Russia
| | - François Lique
- LOMC—UMR 6294, CNRS-Université du Havre, 25 Rue Philippe Lebon, BP 1123, 76 063 Le Havre Cedex, France
| |
Collapse
|
35
|
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]
|
36
|
Abstract
AbstractThis paper provides a brief overview of the journey of molecules through the Cosmos, from local diffuse interstellar clouds and PDRs to distant galaxies, and from cold dark clouds to hot star-forming cores, protoplanetary disks, planetesimals and exoplanets. Recent developments in each area are sketched and the importance of connecting astronomy with chemistry and other disciplines is emphasized. Fourteen challenges for the field of Astrochemistry in the coming decades are formulated.
Collapse
|
37
|
Heritier KL, Altwegg K, Berthelier JJ, Beth A, Carr CM, De Keyser J, Eriksson AI, Fuselier SA, Galand M, Gombosi TI, Henri P, Johansson FL, Nilsson H, Rubin M, Simon Wedlund C, Taylor MGGT, Vigren E. On the origin of molecular oxygen in cometary comae. Nat Commun 2018; 9:2580. [PMID: 29968720 PMCID: PMC6030164 DOI: 10.1038/s41467-018-04972-5] [Citation(s) in RCA: 16] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/28/2017] [Accepted: 06/05/2018] [Indexed: 11/09/2022] Open
Affiliation(s)
- K L Heritier
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK.
| | - K Altwegg
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland
| | | | - A Beth
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK
| | - C M Carr
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK
| | - J De Keyser
- BIRA-IASB, Royal Belgian Institute for Space Aeronomy, Ringlaan 3, Brussels, Belgium
| | - A I Eriksson
- Swedish Institute of Space Physics, Ångström Laboratory, Lägerhyddsvägen 1, 752 37, Uppsala, Sweden
| | - S A Fuselier
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, TX, 78228-0510, USA.,University of Texas at San Antonio, San Antonio, TX, 78249, USA
| | - M Galand
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK
| | - T I Gombosi
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, MI, 48109, USA
| | - P Henri
- LPC2E, CNRS, 3 Avenue de la recherche scientifique, 45071, Orléans, France
| | - F L Johansson
- Swedish Institute of Space Physics, Ångström Laboratory, Lägerhyddsvägen 1, 752 37, Uppsala, Sweden
| | - H Nilsson
- Swedish Institute of Space Physics, P.O. Box 812, 981 28, Kiruna, Sweden
| | - M Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland
| | - C Simon Wedlund
- Department of Physics, University of Oslo, Sem Sælands vei 24, postbox 1048, 0317, Oslo, Norway
| | - M G G T Taylor
- European Space Agency, ESTEC, Keplerlaan 1, Noordwijk, 2200 AG, The Netherlands
| | - E Vigren
- LATMOS/IPSL-CNRS-UPMC-UVSQ, 94100, Saint-Maur, France
| |
Collapse
|
38
|
Yao Y, Giapis KP. Reply to "On the origin of molecular oxygen in cometary comae". Nat Commun 2018; 9:2581. [PMID: 29968721 PMCID: PMC6030084 DOI: 10.1038/s41467-018-04943-w] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/10/2017] [Accepted: 06/05/2018] [Indexed: 11/25/2022] Open
Affiliation(s)
- Y Yao
- Division of Chemistry and Chemical Engineering, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA, 91125, USA
| | - K P Giapis
- Division of Chemistry and Chemical Engineering, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA, 91125, USA.
| |
Collapse
|
39
|
Maté B, Molpeceres G, Tanarro I, Peláez RJ, Guillemin JC, Cernicharo J, Herrero VJ. Stability of CH 3NCO in astronomical ices under energetic processing. A laboratory study. THE ASTROPHYSICAL JOURNAL 2018; 861:61. [PMID: 30185993 PMCID: PMC6120682 DOI: 10.3847/1538-4357/aac826] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
Methyl isocyanate (CH3NCO) was recently found in hot cores and suggested on comet 67P/CG. The incorporation of this molecule into astrochemical networks requires data on its formation and destruction. In this work, ices of pure CH3NCO and of CH3NCO(4-5%)/H2O mixtures deposited at 20 K were irradiated with a UV D2 lamp (120-400 nm) and bombarded by 5 keV electrons to mimic the secondary electrons produced by cosmic rays (CRs). The destruction of CH3NCO was studied using IR spectroscopy. After processing, the νa-NCO band of CH3NCO disappeared and IR bands corresponding to CO, CO2, OCN- and HCN/CN- appeared instead. The products of photon and electron processing were very similar. Destruction cross sections and half-life doses were derived from the measurements. Water ice provides a good shield against UV irradiation (half-life dose of ~ 64 eV molecule-1 for CH3NCO in water-ice), but not so good against high-energy electrons (half-life dose ~ 18 eV molecule-1). It was also found that CH3NCO does not react with H2O over the 20-200 K temperature range. These results indicate that hypothetical CH3NCO in the ices of dense clouds should be stable against UV photons and relatively stable against CRs over the lifetime of a cloud (~ 107 yr), and could sublime in the hot core phase. On the surface of a Kuiper belt object (the original location of comet 67P/CG) the molecule would be swiftly destroyed, both by photons and CRs, but embedded below just 10 μm of water-ice, the molecule could survive for ~ 109 yr.
Collapse
Affiliation(s)
- B. Maté
- Instituto de Estructura de la Materia (IEM-CSIC), Serrano 121-123, 28006 Madrid, Spain
| | - G. Molpeceres
- Instituto de Estructura de la Materia (IEM-CSIC), Serrano 121-123, 28006 Madrid, Spain
| | - I. Tanarro
- Instituto de Estructura de la Materia (IEM-CSIC), Serrano 121-123, 28006 Madrid, Spain
| | - R. J. Peláez
- Instituto de Estructura de la Materia (IEM-CSIC), Serrano 121-123, 28006 Madrid, Spain
| | - J. C. Guillemin
- Univ Rennes, Ecole Nationale Supérieure de Chimie de Rennes, CNRS, ISCR – UMR6226, F-35000 Rennes, France
| | - J. Cernicharo
- Instituto de Física Fundamental (IFF-CSIC), Serrano 121-123, 28006, Madrid, Spain
| | - V. J. Herrero
- Instituto de Estructura de la Materia (IEM-CSIC), Serrano 121-123, 28006 Madrid, Spain
| |
Collapse
|
40
|
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.
Collapse
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
| |
Collapse
|
41
|
Steele EJ, Al-Mufti S, Augustyn KA, Chandrajith R, Coghlan JP, Coulson SG, Ghosh S, Gillman M, Gorczynski RM, Klyce B, Louis G, Mahanama K, Oliver KR, Padron J, Qu J, Schuster JA, Smith WE, Snyder DP, Steele JA, Stewart BJ, Temple R, Tokoro G, Tout CA, Unzicker A, Wainwright M, Wallis J, Wallis DH, Wallis MK, Wetherall J, Wickramasinghe DT, Wickramasinghe JT, Wickramasinghe NC, Liu Y. Cause of Cambrian Explosion - Terrestrial or Cosmic? PROGRESS IN BIOPHYSICS AND MOLECULAR BIOLOGY 2018; 136:3-23. [PMID: 29544820 DOI: 10.1016/j.pbiomolbio.2018.03.004] [Citation(s) in RCA: 26] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/15/2023]
Abstract
We review the salient evidence consistent with or predicted by the Hoyle-Wickramasinghe (H-W) thesis of Cometary (Cosmic) Biology. Much of this physical and biological evidence is multifactorial. One particular focus are the recent studies which date the emergence of the complex retroviruses of vertebrate lines at or just before the Cambrian Explosion of ∼500 Ma. Such viruses are known to be plausibly associated with major evolutionary genomic processes. We believe this coincidence is not fortuitous but is consistent with a key prediction of H-W theory whereby major extinction-diversification evolutionary boundaries coincide with virus-bearing cometary-bolide bombardment events. A second focus is the remarkable evolution of intelligent complexity (Cephalopods) culminating in the emergence of the Octopus. A third focus concerns the micro-organism fossil evidence contained within meteorites as well as the detection in the upper atmosphere of apparent incoming life-bearing particles from space. In our view the totality of the multifactorial data and critical analyses assembled by Fred Hoyle, Chandra Wickramasinghe and their many colleagues since the 1960s leads to a very plausible conclusion - life may have been seeded here on Earth by life-bearing comets as soon as conditions on Earth allowed it to flourish (about or just before 4.1 Billion years ago); and living organisms such as space-resistant and space-hardy bacteria, viruses, more complex eukaryotic cells, fertilised ova and seeds have been continuously delivered ever since to Earth so being one important driver of further terrestrial evolution which has resulted in considerable genetic diversity and which has led to the emergence of mankind.
Collapse
Affiliation(s)
- Edward J Steele
- CY O'Connor ERADE Village Foundation, Piara Waters, WA, Australia; Centre for Astrobiology, University of Ruhuna, Matara, Sri Lanka.
| | - Shirwan Al-Mufti
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - Kenneth A Augustyn
- Center for the Physics of Living Organisms, Department of Physics, Michigan Technological University, Michigan, United States
| | | | - John P Coghlan
- University of Melbourne, Office of the Dean, Faculty Medicine, Dentistry and Health Sciences, 3rd Level, Alan Gilbert Building, Australia
| | - S G Coulson
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - Sudipto Ghosh
- Metallurgical & Materials Engineering IIT, Kanpur, India
| | - Mark Gillman
- South African Brain Research Institute, 6 Campbell Street, Waverly, Johannesburg, South Africa
| | - Reginald M Gorczynski
- University Toronto Health Network, Toronto General Hospital, University of Toronto, Canada
| | - Brig Klyce
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - Godfrey Louis
- Department of Physics, Cochin University of Science and Technology Cochin, India
| | | | - Keith R Oliver
- School of Veterinary and Life Sciences Murdoch University, Perth, WA, Australia
| | - Julio Padron
- Studio Eutropi, Clinical Pathology and Nutrition, Via Pompei 46, Ardea, 00040, Rome, Italy
| | - Jiangwen Qu
- Department of Infectious Disease Control, Tianjin Center for Disease Control and Prevention, China
| | - John A Schuster
- School of History and Philosophy of Science, Faculty of Science, University of Sydney, Sydney, Australia
| | - W E Smith
- Institute for the Study of Panspermia and Astrobiology, Gifu, Japan
| | - Duane P Snyder
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - Julian A Steele
- Centre for Surface Chemistry and Catalysis, KU Leuven, Celestijnenlaan 200F, 3001, Leuven, Belgium
| | - Brent J Stewart
- CY O'Connor ERADE Village Foundation, Piara Waters, WA, Australia
| | - Robert Temple
- The History of Chinese Culture Foundation, Conway Hall, London, UK
| | - Gensuke Tokoro
- Institute for the Study of Panspermia and Astrobiology, Gifu, Japan
| | - Christopher A Tout
- Institute of Astronomy, The Observatories, Madingley Road, Cambridge, CB3 0HA, UK
| | | | - Milton Wainwright
- Buckingham Centre for Astrobiology, University of Buckingham, UK; Centre for Astrobiology, University of Ruhuna, Matara, Sri Lanka
| | - Jamie Wallis
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - Daryl H Wallis
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - Max K Wallis
- Buckingham Centre for Astrobiology, University of Buckingham, UK
| | - John Wetherall
- School of Biomedical Sciences, Perth, Curtin University, WA, Australia
| | - D T Wickramasinghe
- College of Physical and Mathematical Sciences, Australian National University, Canberra, Australia
| | | | - N Chandra Wickramasinghe
- Buckingham Centre for Astrobiology, University of Buckingham, UK; Centre for Astrobiology, University of Ruhuna, Matara, Sri Lanka; Institute for the Study of Panspermia and Astrobiology, Gifu, Japan
| | - Yongsheng Liu
- Henan Collaborative Innovation Center of Modern Biological Breeding, Henan Institute of Science and Technology, Xinxiang, 453003, China; Department of Biochemistry, University of Alberta, Edmonton, AB T6G 2H7, Canada
| |
Collapse
|
42
|
Yang T, Thomas AM, Dangi BB, Kaiser RI, Mebel AM, Millar TJ. Directed gas phase formation of silicon dioxide and implications for the formation of interstellar silicates. Nat Commun 2018; 9:774. [PMID: 29472549 PMCID: PMC5823853 DOI: 10.1038/s41467-018-03172-5] [Citation(s) in RCA: 17] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/01/2017] [Accepted: 01/24/2018] [Indexed: 11/12/2022] Open
Abstract
Interstellar silicates play a key role in star formation and in the origin of solar systems, but their synthetic routes have remained largely elusive so far. Here we demonstrate in a combined crossed molecular beam and computational study that silicon dioxide (SiO2) along with silicon monoxide (SiO) can be synthesized via the reaction of the silylidyne radical (SiH) with molecular oxygen (O2) under single collision conditions. This mechanism may provide a low-temperature path-in addition to high-temperature routes to silicon oxides in circumstellar envelopes-possibly enabling the formation and growth of silicates in the interstellar medium necessary to offset the fast silicate destruction.
Collapse
Affiliation(s)
- Tao Yang
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI, 96822, USA
- State Key Laboratory of Precision Spectroscopy, East China Normal University, Shanghai, 200062, China
| | - Aaron M Thomas
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI, 96822, USA
| | - Beni B Dangi
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI, 96822, USA
- Department of Chemistry, Florida Agricultural and Mechanical University, Tallahassee, FL, 32307, USA
| | - Ralf I Kaiser
- Department of Chemistry, University of Hawai'i at Mānoa, Honolulu, HI, 96822, USA.
| | - Alexander M Mebel
- Department of Chemistry and Biochemistry, Florida International University, Miami, FL, 33199, USA.
| | - Tom J Millar
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, BT7 1NN, UK.
| |
Collapse
|
43
|
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.
Collapse
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.
| |
Collapse
|
44
|
Westbrook BR, Dreux KM, Tschumper GS, Francisco JS, Fortenberry RC. Binding of the atomic cations hydrogen through argon to water and hydrogen sulfide. Phys Chem Chem Phys 2018; 20:25967-25973. [DOI: 10.1039/c8cp05378b] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
Water and hydrogen sulfide will bind with every atomic cation from the first three rows of the periodic table.
Collapse
Affiliation(s)
| | - Katelyn M. Dreux
- Department of Chemistry and Biochemistry
- University of Mississippi
- USA
| | | | - Joseph S. Francisco
- Department of Earth and Environmental Science Philadelphia
- University of Pennsylvania
- USA
| | | |
Collapse
|
45
|
Rosetta Mission: Electron Scattering Cross Sections—Data Needs and Coverage in BEAMDB Database. ATOMS 2017. [DOI: 10.3390/atoms5040046] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
|
46
|
Tsegaw YA, Góbi S, Förstel M, Maksyutenko P, Sander W, Kaiser RI. Formation of Hydroxylamine in Low-Temperature Interstellar Model Ices. J Phys Chem A 2017; 121:7477-7493. [PMID: 28892389 DOI: 10.1021/acs.jpca.7b07500] [Citation(s) in RCA: 16] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Affiliation(s)
- Yetsedaw A. Tsegaw
- Lehrstuhl
für Organische Chemie II, Ruhr-Universität Bochum, 44780 Bochum, Germany
| | | | | | | | - Wolfram Sander
- Lehrstuhl
für Organische Chemie II, Ruhr-Universität Bochum, 44780 Bochum, Germany
| | | |
Collapse
|
47
|
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'.
Collapse
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
| |
Collapse
|
48
|
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'.
Collapse
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
| |
Collapse
|
49
|
A'Hearn MF. Comets: looking ahead. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2016.0261. [PMID: 28554980 PMCID: PMC5454229 DOI: 10.1098/rsta.2016.0261] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 10/06/2016] [Indexed: 05/25/2023]
Abstract
We outline the key questions about comets that must be answered in order to understand cometary formation in the context of the protoplanetary disc and the role of comets in the formation and evolution of the solar system. We then discuss the new understanding of comets from Rosetta and from other recent advances, including work presented by others at the discussion meeting. Finally, we suggest some key directions for future projects to better address the above questions.This article is part of the themed issue 'Cometary science after Rosetta'.
Collapse
Affiliation(s)
- Michael F A'Hearn
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA
| |
Collapse
|
50
|
Marty B, Altwegg K, Balsiger H, Bar-Nun A, Bekaert DV, Berthelier JJ, Bieler A, Briois C, Calmonte U, Combi M, De Keyser J, Fiethe B, Fuselier SA, Gasc S, Gombosi TI, Hansen KC, Hässig M, Jäckel A, Kopp E, Korth A, Le Roy L, Mall U, Mousis O, Owen T, Rème H, Rubin M, Sémon T, Tzou CY, Waite JH, Wurz P. Xenon isotopes in 67P/Churyumov-Gerasimenko show that comets contributed to Earth's atmosphere. Science 2017; 356:1069-1072. [DOI: 10.1126/science.aal3496] [Citation(s) in RCA: 131] [Impact Index Per Article: 18.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/05/2016] [Accepted: 05/03/2017] [Indexed: 11/02/2022]
Affiliation(s)
- B. Marty
- Centre de Recherches Pétrographiques et Géochimiques, CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre lès Nancy, France
| | - 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
| | - D. V. Bekaert
- Centre de Recherches Pétrographiques et Géochimiques, CNRS, Université de Lorraine, 15 rue Notre Dame des Pauvres, BP 20, 54501 Vandoeuvre lès Nancy, France
| | - J.-J. Berthelier
- Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Institut Pierre Simon Laplace, CNRS, Université Pierre et Marie Curie, 4 Avenue de Neptune, 94100 Saint-Maur, France
| | - A. Bieler
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - C. Briois
- Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E), UMR 6115 CNRS–Université d’Orléans, France
| | - U. Calmonte
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - M. Combi
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - J. De Keyser
- Koninklijk Belgisch Instituut voor Ruimte-Aeronomie/Institut Royal d’Aéronomie Spatiale de Belgique (BIRA-IASB), Ringlaan 3, B-1180 Brussels, Belgium
| | - B. Fiethe
- Institute of Computer and Network Engineering (IDA), 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 Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, USA
| | - K. C. Hansen
- Department of Climate and Space Sciences and Engineering, University of Michigan, 2455 Hayward Street, 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 (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - L. Le Roy
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - U. Mall
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - O. Mousis
- Laboratoire d’Astrophysique de Marseille, CNRS, Aix Marseille Université, 13388 Marseille, France
| | - T. Owen
- Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA
| | - H. 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
| | - M. Rubin
- Physikalisches Institut, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | - 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
| |
Collapse
|