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Kirchschlager F, Mattsson L, Gent FA. Supernova dust destruction in the magnetized turbulent ISM. Nat Commun 2024; 15:1841. [PMID: 38418455 PMCID: PMC10901883 DOI: 10.1038/s41467-024-45962-0] [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: 06/29/2023] [Accepted: 02/07/2024] [Indexed: 03/01/2024] Open
Abstract
Dust in the interstellar medium (ISM) is critical to the absorption and intensity of emission profiles used widely in astronomical observations, and necessary for star and planet formation. Supernovae (SNe) both produce and destroy ISM dust. In particular the destruction rate is difficult to assess. Theory and prior simulations of dust processing by SNe in a uniform ISM predict quite high rates of dust destruction, potentially higher than the supernova dust production rate in some cases. Here we show simulations of supernova-induced dust processing with realistic ISM dynamics including magnetic field effects and demonstrate how ISM inhomogeneity and magnetic fields inhibit dust destruction. Compared to the non-magnetic homogeneous case, the dust mass destroyed within 1 Myr per SNe is reduced by more than a factor of two, which can have a great impact on the ISM dust budget.
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Affiliation(s)
- Florian Kirchschlager
- Physics and Astronomy, Ghent University, Krijgslaan 281-S9, Ghent, 9000, Belgium
- Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
| | - Lars Mattsson
- Nordita, KTH Royal Institute of Technology and Stockholm University, Hannes Alfvéns väg 12, Stockholm, SE-106, Sweden.
| | - Frederick A Gent
- Nordita, KTH Royal Institute of Technology and Stockholm University, Hannes Alfvéns väg 12, Stockholm, SE-106, Sweden
- Astroinformatics, Computer Science, Aalto University, PO Box 15399, Espoo, FI-00076, Finland
- School of Mathematics, Statistics and Physics, Newcastle University, Newcastle, NE1 7RU, UK
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2
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Fransson C, Barlow MJ, Kavanagh PJ, Larsson J, Jones OC, Sargent B, Meixner M, Bouchet P, Temim T, Wright GS, Blommaert JADL, Habel N, Hirschauer AS, Hjorth J, Lenkić L, Tikkanen T, Wesson R, Coulais A, Fox OD, Gastaud R, Glasse A, Jaspers J, Krause O, Lau RM, Nayak O, Rest A, Colina L, van Dishoeck EF, Güdel M, Henning T, Lagage PO, Östlin G, Ray TP, Vandenbussche B. Emission lines due to ionizing radiation from a compact object in the remnant of Supernova 1987A. Science 2024; 383:898-903. [PMID: 38386759 DOI: 10.1126/science.adj5796] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/06/2023] [Accepted: 01/12/2024] [Indexed: 02/24/2024]
Abstract
The nearby Supernova 1987A was accompanied by a burst of neutrino emission, which indicates that a compact object (a neutron star or black hole) was formed in the explosion. There has been no direct observation of this compact object. In this work, we observe the supernova remnant with JWST spectroscopy, finding narrow infrared emission lines of argon and sulfur. The line emission is spatially unresolved and blueshifted in velocity relative to the supernova rest frame. We interpret the lines as gas illuminated by a source of ionizing photons located close to the center of the expanding ejecta. Photoionization models show that the line ratios are consistent with ionization by a cooling neutron star or a pulsar wind nebula. The velocity shift could be evidence for a neutron star natal kick.
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Affiliation(s)
- C Fransson
- Department of Astronomy, Stockholm University, The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
| | - M J Barlow
- Department of Physics and Astronomy, University College London, London WC1E 6BT, UK
| | - P J Kavanagh
- Department of Experimental Physics, Maynooth University, Maynooth, County Kildare, Ireland
- Astronomy & Astrophyics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Ireland
| | - J Larsson
- Department of Physics, KTH Royal Institute of Technology, The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
| | - O C Jones
- UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - B Sargent
- Space Telescope Science Institute, Baltimore, MD 21218, USA
- Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
| | - M Meixner
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - P Bouchet
- Université Paris-Saclay, Université Paris Cité, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Centre National de la Recherche Scientifique, Astrophysique Instrumentation Modélisation, Saint Aubin, France
| | - T Temim
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - G S Wright
- UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - J A D L Blommaert
- Astronomy and Astrophysics Research Group, Department of Physics and Astrophysics, Vrije Universiteit Brussel, B-1050 Brussels, Belgium
| | - N Habel
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - A S Hirschauer
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - J Hjorth
- Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, 2200 Copenhagen, Denmark
| | - L Lenkić
- Stratospheric Observatory for Infrared Astronomy Science Center, Universities Space Research Association, NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - T Tikkanen
- School of Physics and Astronomy, Space Research Centre, Space Park Leicester, University of Leicester, Leicester LE4 5SP, UK
| | - R Wesson
- School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
| | - A Coulais
- Université Paris-Saclay, Université Paris Cité, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Centre National de la Recherche Scientifique, Astrophysique Instrumentation Modélisation, Saint Aubin, France
- Laboratoire d'Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères, Observatoire de Paris, Paris Sciences et Lettres Research University, National Centre for Scientific Research, Sorbonne Université, Paris, France
| | - O D Fox
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - R Gastaud
- Université Paris-Saclay, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Detectors Electronics and Computing for Physics, Gif-sur-Yvette, France
| | - A Glasse
- UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - J Jaspers
- Department of Experimental Physics, Maynooth University, Maynooth, County Kildare, Ireland
- Astronomy & Astrophyics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Ireland
| | - O Krause
- Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
| | - R M Lau
- National Optical-Infrared Astronomy Research Laboratory, National Science Foundation, Tucson, AZ 85719, USA
| | - O Nayak
- NASA Goddard Space Flight Center, Greenbelt, MD 20770, USA
| | - A Rest
- Space Telescope Science Institute, Baltimore, MD 21218, USA
- Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
| | - L Colina
- Centro de Astrobiología, Consejo Superior de Investigaciones Científicas - Instituto Nacional de Técnica Aeroespacial, Torrejón de Ardoz, E-28850, Madrid, Spain
| | - E F van Dishoeck
- Max-Planck Institut für Extraterrestrische Physik, D-85748 Garching, Germany
- Leiden Observatory, 2300 RA Leiden, Netherlands
| | - M Güdel
- Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
- Department of Astrophysics, University of Vienna, A-1180 Vienna, Austria
- Institute for Particle Physics and Astrophysics, Eidgenössische Technische Hochschule Zürich, 8093 Zürich, Switzerland
| | - Th Henning
- Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
| | - P-O Lagage
- Université Paris-Saclay, Université Paris Cité, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Centre National de la Recherche Scientifique, Astrophysique Instrumentation Modélisation, Saint Aubin, France
| | - G Östlin
- Department of Astronomy, Stockholm University, The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
| | - T P Ray
- Astronomy & Astrophyics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Ireland
| | - B Vandenbussche
- Institute of Astronomy, Katholieke Universiteit Leuven, 3001 Leuven, Belgium
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Wang王 L灵, Hu M, Wang L, Yang 杨 Y轶, Yang J, Gomez H, Chen S, Hu L, Chen TW, Mo J, Wang X, Baade D, Hoeflich P, Wheeler JC, Pignata G, Burke J, Hiramatsu D, Howell DA, McCully C, Pellegrino C, Galbany L, Hsiao EY, Sand DJ, Zhang J, Uddin SA, Anderson JP, Ashall C, Cheng C, Gromadzki M, Inserra C, Lin H, Morrell N, Morales-Garoffolo A, Müller-Bravo TE, Nicholl M, Gonzalez EP, Phillips MM, Pineda-García J, Sai H, Smith M, Shahbandeh M, Srivastav S, Stritzinger MD, Yang S, Young DR, Yu L, Zhang X. Newly formed dust within the circumstellar environment of SN Ia-CSM 2018evt. NATURE ASTRONOMY 2024; 8:504-519. [PMID: 38659610 PMCID: PMC11035149 DOI: 10.1038/s41550-024-02197-9] [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: 11/11/2022] [Accepted: 01/05/2024] [Indexed: 04/26/2024]
Abstract
Dust associated with various stellar sources in galaxies at all cosmic epochs remains a controversial topic, particularly whether supernovae play an important role in dust production. We report evidence of dust formation in the cold, dense shell behind the ejecta-circumstellar medium (CSM) interaction in the Type Ia-CSM supernova (SN) 2018evt three years after the explosion, characterized by a rise in mid-infrared emission accompanied by an accelerated decline in the optical radiation of the SN. Such a dust-formation picture is also corroborated by the concurrent evolution of the profiles of the Hα emission line. Our model suggests enhanced CSM dust concentration at increasing distances from the SN as compared to what can be expected from the density profile of the mass loss from a steady stellar wind. By the time of the last mid-infrared observations at day +1,041, a total amount of 1.2 ± 0.2 × 10-2 M⊙ of new dust has been formed by SN 2018evt, making SN 2018evt one of the most prolific dust factories among supernovae with evidence of dust formation. The unprecedented witness of the intense production procedure of dust may shed light on the perceptions of dust formation in cosmic history.
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Grants
- National Natural Science Foundation of China (National Science Foundation of China)
- This work is sponsored (in part) by the Chinese Academy of Sciences (CAS), through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile
- the Major Science and Technology Project of Qinghai Province (2019-ZJ-A10) and the Jiangsu Funding Program for Excellent Postdoctoral Talent.
- National Science Foundation (NSF)
- Y.Y. appreciates the generous financial support provided to the supernova group at U.C. Berkeley (PI: Alexei V. Filippenko) by Gary and Cynthia Bengier, Clark and Sharon Winslow, Sanford Robertson, and numerous other donors.
- China Postdoctoral Science Foundation
- L.H. acknowledges support from Jiangsu Funding Program for Excellent Postdoctoral Talent.
- T.W.C. acknowledges the Yushan Young Fellow Program by the Ministry of Education, Taiwan for the financial support.
- a DOE grant to the Wooten Center for Astrophysical Plasma Properties (WCAPP; PI Don Winget), and by grant G09-20065C from the Chandra Observatory.
- Millennium Science Initiative ICN12_009
- Spanish Ministerio de Ciencia e Innovaci\'on (MCIN), the Agencia Estatal de Investigaci\'on (AEI) 10.13039/501100011033, and the European Social Fund (ESF) "Investing in your future" under the 2019 Ram\'on y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cient\'ificas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Mar\'ia de Maeztu CEX2020-001058-M
- EU Horizon 2020 research and innovation programme under grant agreement No 101004719
- European Union under the 2014-2020 ERDF Operational Programme and by the Department of Economic Transformation, Industry, Knowledge, and Universities of the Regional Government of Andalusia through the FEDER-UCA18-107404 grant
- Spanish Ministerio de Ciencia e Innovaci\'on (MCIN), the Agencia Estatal de Investigaci\'on (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cient\'ificas (CSIC) under the PIE project 20215AT016 and the I-LINK 2021 LINKA20409, and the program Unidad de Excelencia Mar\'ia de Maeztu CEX2020-001058-M.
- European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No.~948381) and by a Fellowship from the Alan Turing Institute.
- a visiting astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration
- Chinese Academy of Sciences (CAS), through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile
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Affiliation(s)
- Lingzhi 灵芝 Wang王
- Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories, CAS, Beijing, China
- CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Maokai Hu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
| | - Lifan Wang
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - Yi 轶 Yang 杨
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
- Department of Astronomy, University of California, Berkeley, CA USA
| | - Jiawen Yang
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - Haley Gomez
- Cardiff Hub for Astrophysics Research and Technology, School of Physics & Astronomy, Cardiff University, Cardiff, UK
| | - Sijie Chen
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - Lei Hu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA USA
| | - Ting-Wan Chen
- Graduate Institute of Astronomy, National Central University, Jhongli, Taiwan
| | - Jun Mo
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
| | - Xiaofeng Wang
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
- Beijing Planetarium, Beijing Academy of Science and Technology, Beijing, China
| | - Dietrich Baade
- European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Garching b. München, Germany
| | - Peter Hoeflich
- Department of Physics, Florida State University, Tallahassee, FL USA
| | | | - Giuliano Pignata
- Instituto de Alta Investigación, Universidad de Tarapacá, Arica, Chile
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
| | - Jamison Burke
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | - Daichi Hiramatsu
- Center for Astrophysics, Harvard & Smithsonian, Cambridge, MA USA
- The NSF AI Institute for Artificial Intelligence and Fundamental Interactions, Alexandria, VA USA
| | - D. Andrew Howell
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | | | - Craig Pellegrino
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | - Lluís Galbany
- Institute of Space Sciences (ICE, CSIC), Barcelona, Spain
- Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - Eric Y. Hsiao
- Department of Physics, Florida State University, Tallahassee, FL USA
| | - David J. Sand
- Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ USA
| | - Jujia Zhang
- Yunnan Observatories, Chinese Academy of Sciences, Kunming, China
| | - Syed A. Uddin
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - J. P. Anderson
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
- European Southern Observatory, Santiago, Chile
| | - Chris Ashall
- Department of Physics, Virginia Tech, Blacksburg, VA USA
| | - Cheng Cheng
- Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories, CAS, Beijing, China
| | | | - Cosimo Inserra
- Cardiff Hub for Astrophysics Research and Technology, School of Physics & Astronomy, Cardiff University, Cardiff, UK
| | - Han Lin
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
| | - N. Morrell
- Carnegie Observatories, Las Campanas Observatory, La Serena, Chile
| | | | - T. E. Müller-Bravo
- Institute of Space Sciences (ICE, CSIC), Barcelona, Spain
- Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - Matt Nicholl
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, UK
| | - Estefania Padilla Gonzalez
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | - M. M. Phillips
- Carnegie Observatories, Las Campanas Observatory, La Serena, Chile
| | - J. Pineda-García
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
- Departamento de Ciencias Físicas, Universidad Andres Bello, Santiago, Chile
| | - Hanna Sai
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
| | - Mathew Smith
- Université de Lyon, Université Claude Bernard Lyon 1, Villeurbanne, France
| | - M. Shahbandeh
- Space Telescope Science Institute, Baltimore, MD USA
| | - Shubham Srivastav
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, UK
| | - M. D. Stritzinger
- Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark
| | - Sheng Yang
- Henan Academy of Sciences, Zhengzhou, China
| | - D. R. Young
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, UK
| | - Lixin Yu
- Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories, CAS, Beijing, China
| | - Xinghan Zhang
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
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Wallner A, Froehlich MB, Hotchkis MAC, Kinoshita N, Paul M, Martschini M, Pavetich S, Tims SG, Kivel N, Schumann D, Honda M, Matsuzaki H, Yamagata T. 60Fe and 244Pu deposited on Earth constrain the r-process yields of recent nearby supernovae. Science 2021; 372:742-745. [PMID: 33986180 DOI: 10.1126/science.aax3972] [Citation(s) in RCA: 21] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/21/2019] [Accepted: 04/12/2021] [Indexed: 11/02/2022]
Abstract
Half of the chemical elements heavier than iron are produced by the rapid neutron capture process (r-process). The sites and yields of this process are disputed, with candidates including some types of supernovae (SNe) and mergers of neutron stars. We search for two isotopic signatures in a sample of Pacific Ocean crust-iron-60 (60Fe) (half-life, 2.6 million years), which is predominantly produced in massive stars and ejected in supernova explosions, and plutonium-244 (244Pu) (half-life, 80.6 million years), which is produced solely in r-process events. We detect two distinct influxes of 60Fe to Earth in the last 10 million years and accompanying lower quantities of 244Pu. The 244Pu/60Fe influx ratios are similar for both events. The 244Pu influx is lower than expected if SNe dominate r-process nucleosynthesis, which implies some contribution from other sources.
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Affiliation(s)
- A Wallner
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia. .,Helmholtz-Zentrum Dresden-Rossendorf, Institute of Ion Beam Physics and Materials Research, 01328 Dresden, Germany
| | - M B Froehlich
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - M A C Hotchkis
- Australian Nuclear Science and Technology Organisation, Lucas Heights, NSW 2234, Australia
| | - N Kinoshita
- Institute of Technology, Shimizu Corporation, Tokyo 135-8530, Japan
| | - M Paul
- Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - M Martschini
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - S Pavetich
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - S G Tims
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - N Kivel
- Laboratory of Radiochemistry, Department for Nuclear Energy and Safety, Paul Scherrer Institute, 5232 Villigen, Switzerland
| | - D Schumann
- Laboratory of Radiochemistry, Department for Nuclear Energy and Safety, Paul Scherrer Institute, 5232 Villigen, Switzerland
| | - M Honda
- Graduate School of Pure and Applied Sciences, University of Tsukuba, Ibaraki 305-8577, Japan
| | - H Matsuzaki
- Micro Analysis Laboratory, Tandem Accelerator, The University Museum, The University of Tokyo, Tokyo 113-0032, Japan
| | - T Yamagata
- Micro Analysis Laboratory, Tandem Accelerator, The University Museum, The University of Tokyo, Tokyo 113-0032, Japan
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The Origin of Cosmic Rays: How Their Composition Defines Their Sources and Sites and the Processes of Their Mixing, Injection, and Acceleration. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4365/ab4b58] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Liu N, Nittler LR, Alexander CMO, Wang J. Late formation of silicon carbide in type II supernovae. SCIENCE ADVANCES 2018; 4:eaao1054. [PMID: 29376119 PMCID: PMC5777395 DOI: 10.1126/sciadv.aao1054] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 06/14/2017] [Accepted: 12/13/2017] [Indexed: 06/07/2023]
Abstract
We have found that individual presolar silicon carbide (SiC) dust grains from supernovae show a positive correlation between 49Ti and 28Si excesses, which is attributed to the radioactive decay of the short-lived (t½ = 330 days) 49V to 49Ti in the inner highly 28Si-rich Si/S zone. The 49V-49Ti chronometer shows that these supernova SiC dust grains formed at least 2 years after their parent stars exploded. This result supports recent dust condensation calculations that predict a delayed formation of carbonaceous and SiC grains in supernovae. The astronomical observation of continuous buildup of dust in supernovae over several years can, therefore, be interpreted as a growing addition of C-rich dust to the dust reservoir in supernovae.
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Kimura Y, Tanaka KK, Nozawa T, Takeuchi S, Inatomi Y. Pure iron grains are rare in the universe. SCIENCE ADVANCES 2017; 3:e1601992. [PMID: 28116359 PMCID: PMC5242559 DOI: 10.1126/sciadv.1601992] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/23/2016] [Accepted: 11/30/2016] [Indexed: 06/06/2023]
Abstract
The abundant forms in which the major elements in the universe exist have been determined from numerous astronomical observations and meteoritic analyses. Iron (Fe) is an exception, in that only depletion of gaseous Fe has been detected in the interstellar medium, suggesting that Fe is condensed into a solid, possibly the astronomically invisible metal. To determine the primary form of Fe, we replicated the formation of Fe grains in gaseous ejecta of evolved stars by means of microgravity experiments. We found that the sticking probability for the formation of Fe grains is extremely small; only a few atoms will stick per hundred thousand collisions so that homogeneous nucleation of metallic Fe grains is highly ineffective, even in the Fe-rich ejecta of type Ia supernovae. This implies that most Fe is locked up as grains of Fe compounds or as impurities accreted onto other grains in the interstellar medium.
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Affiliation(s)
- Yuki Kimura
- Institute of Low Temperature Science, Hokkaido University, Sapporo 060-0819, Japan
| | - Kyoko K. Tanaka
- Institute of Low Temperature Science, Hokkaido University, Sapporo 060-0819, Japan
| | - Takaya Nozawa
- Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
| | - Shinsuke Takeuchi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan
| | - Yuko Inatomi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan
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Dwek E. IRON: A KEY ELEMENT FOR UNDERSTANDING THE ORIGIN AND EVOLUTION OF INTERSTELLAR DUST. THE ASTROPHYSICAL JOURNAL 2016; 825:136. [PMID: 32747835 PMCID: PMC7398334 DOI: 10.3847/0004-637x/825/2/136] [Citation(s) in RCA: 42] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
The origin and depletion of iron differ from all other abundant refractory elements that make up the composition of the interstellar dust. Iron is primarily synthesized in Type Ia supernovae (SNe Ia) and in core collapse supernovae (CCSN), and is present in the outflows from AGB stars. Only the latter two are observed to be sources of interstellar dust, since searches for dust in SN Ia have provided strong evidence for the absence of any significant mass of dust in their ejecta. Consequently, more than 65% of the iron is injected into the ISM in gaseous form. Yet, ultraviolet and X-ray observations along many lines of sight in the ISM show that iron is severely depleted in the gas phase compared to expected solar abundances. The missing iron, comprising about 90% of the total, is believed to be locked up in interstellar dust. This suggests that most of the missing iron must have precipitated from the ISM gas by cold accretion onto preexisting silicate, carbon, or composite grains. Iron is thus the only element that requires most of its growth to occur outside the traditional stellar condensation sources. This is a robust statement that does not depend on our evolving understanding of the dust destruction efficiency in the ISM. Reconciling the physical, optical, and chemical properties of such composite grains with their many observational manifestations is a major challenge for understanding the nature and origin of interstellar dust.
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Affiliation(s)
- Eli Dwek
- Observational Cosmology Lab., Code 665 NASA Goddard Space Flight Center, Greenbelt, MD 20771
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Cernicharo J, McCarthy MC, Gottlieb CA, Agúndez M, Velilla Prieto L, Baraban JH, Changala PB, Guélin M, Kahane C, Martin-Drumel MA, Patel NA, Reilly NJ, Stanton JF, Quintana-Lacaci G, Thorwirth S, Young KH. Discovery of SiCSi in IRC +10216: A missing link between gas and dust carriers of Si-C bonds. THE ASTROPHYSICAL JOURNAL. LETTERS 2015; 806:L3. [PMID: 26722621 PMCID: PMC4693961 DOI: 10.1088/2041-8205/806/1/l3] [Citation(s) in RCA: 62] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
We report the discovery in space of a disilicon species, SiCSi, from observations between 80 and 350 GHz with the IRAM 30m radio telescope. Owing to the close coordination between laboratory experiments and astrophysics, 112 lines have now been detected in the carbon-rich star CW Leo. The derived frequencies yield improved rotational and centrifugal distortion constants up to sixth order. From the line profiles and interferometric maps with the Submillimeter Array, the bulk of the SiCSi emission arises from a region of 6″ in radius. The derived abundance is comparable to that of SiC2. As expected from chemical equilibrium calculations, SiCSi and SiC2 are the most abundant species harboring a Si-C bond in the dust formation zone and certainly both play a key role in the formation of SiC dust grains.
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Affiliation(s)
- J Cernicharo
- Group of Molecular Astrophysics. ICMM. CSIC. C/Sor Juana Inés de La Cruz N3. E-28049, Madrid. Spain
| | - M C McCarthy
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138
| | - C A Gottlieb
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138
| | - M Agúndez
- Group of Molecular Astrophysics. ICMM. CSIC. C/Sor Juana Inés de La Cruz N3. E-28049, Madrid. Spain
| | - L Velilla Prieto
- Group of Molecular Astrophysics. ICMM. CSIC. C/Sor Juana Inés de La Cruz N3. E-28049, Madrid. Spain
| | - J H Baraban
- Department of Chemistry and Biochemistry, University of Colorado, Boulder, CO 80309
| | - P B Changala
- JILA, National Institute of Standards and Technology and University of Colorado, and Department of Physics, University of Colorado, Boulder, CO 80309
| | - M Guélin
- Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, F-38406, St-Martin d'Hères, France
| | - C Kahane
- Universit Grenoble Alpes, IPAG, F-38000 Grenoble, France; CNRS, IPAG, F-38000 Grenoble, France
| | - M A Martin-Drumel
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138
| | - N A Patel
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138
| | - N J Reilly
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138
| | - J F Stanton
- Institute for Theoretical Chemistry, Department of Chemistry, The University of Texas at Austin, Austin, TX 78712
| | - G Quintana-Lacaci
- Group of Molecular Astrophysics. ICMM. CSIC. C/Sor Juana Inés de La Cruz N3. E-28049, Madrid. Spain
| | - S Thorwirth
- I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
| | - K H Young
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, and School of Engineering & Applied Sciences, Harvard University, Cambridge, MA 02138
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11
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Lau RM, Herter TL, Morris MR, Li Z, Adams JD. Supernovae. Old supernova dust factory revealed at the Galactic center. Science 2015; 348:413-8. [PMID: 25791082 DOI: 10.1126/science.aaa2208] [Citation(s) in RCA: 34] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/05/2014] [Accepted: 03/06/2015] [Indexed: 11/02/2022]
Abstract
Dust formation in supernova ejecta is currently the leading candidate to explain the large quantities of dust observed in the distant, early universe. However, it is unclear whether the ejecta-formed dust can survive the hot interior of the supernova remnant (SNR). We present infrared observations of ~0.02 solar masses of warm (~100 kelvin) dust seen near the center of the ~10,000-year-old Sagittarius A East SNR at the Galactic center. Our findings indicate the detection of dust within an older SNR that is expanding into a relatively dense surrounding medium (electron density ~10(3) centimeters(-3)) and has survived the passage of the reverse shock. The results suggest that supernovae may be the dominant dust-production mechanism in the dense environment of galaxies of the early universe.
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Affiliation(s)
- R M Lau
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA.
| | - T L Herter
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
| | - M R Morris
- Department of Physics and Astronomy, University of California, Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
| | - Z Li
- School of Astronomy and Space Science, Nanjing University, 22 Hankou Road, Nanjing, Jiangsu 210093, China
| | - J D Adams
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA. Stratospheric Observatory for Infrared Astronomy (SOFIA) Science Center, Universities Space Research Association, NASA Ames Research Center, MS 232, Moffett Field, CA 94035, USA
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12
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13
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Schiller M, Paton C, Bizzarro M. Evidence for nucleosynthetic enrichment of the protosolar molecular cloud core by multiple supernova events. GEOCHIMICA ET COSMOCHIMICA ACTA 2015; 149:88-102. [PMID: 25684790 PMCID: PMC4326683 DOI: 10.1016/j.gca.2014.11.005] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
The presence of isotope heterogeneity of nucleosynthetic origin amongst meteorites and their components provides a record of the diverse stars that contributed matter to the protosolar molecular cloud core. Understanding how and when the solar system's nucleosynthetic heterogeneity was established and preserved within the solar protoplanetary disk is critical for unraveling the earliest formative stages of the solar system. Here, we report calcium and magnesium isotope measurements of primitive and differentiated meteorites as well as various types of refractory inclusions, including refractory inclusions (CAIs) formed with the canonical 26Al/27Al of ~5 × 10-5 (26Al decays to 26Mg with a half-life of ~0.73 Ma) and CAIs that show fractionated and unidentified nuclear effects (FUN-CAIs) to understand the origin of the solar system's nucleosynthetic heterogeneity. Bulk analyses of primitive and differentiated meteorites along with canonical and FUN-CAIs define correlated, mass-independent variations in 43Ca, 46Ca and 48Ca. Moreover, sequential dissolution experiments of the Ivuna carbonaceous chondrite aimed at identifying the nature and number of presolar carriers of isotope anomalies within primitive meteorites have detected the presence of multiple carriers of the short-lived 26Al nuclide as well as carriers of anomalous and uncorrelated 43Ca, 46Ca and 48Ca compositions, which requires input from multiple and recent supernovae sources. We infer that the solar system's correlated nucleosynthetic variability reflects unmixing of old, galactically-inherited homogeneous dust from a new, supernovae-derived dust component formed shortly prior to or during the evolution of the giant molecular cloud parental to the protosolar molecular cloud core. This implies that similarly to 43Ca, 46Ca and 48Ca, the short-lived 26Al nuclide was heterogeneously distributed in the inner solar system at the time of CAI formation.
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14
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Rapid formation of large dust grains in the luminous supernova 2010jl. Nature 2014; 511:326-9. [PMID: 25030169 DOI: 10.1038/nature13558] [Citation(s) in RCA: 140] [Impact Index Per Article: 14.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/12/2013] [Accepted: 05/29/2014] [Indexed: 11/08/2022]
Abstract
The origin of dust in galaxies is still a mystery. The majority of the refractory elements are produced in supernova explosions, but it is unclear how and where dust grains condense and grow, and how they avoid destruction in the harsh environments of star-forming galaxies. The recent detection of 0.1 to 0.5 solar masses of dust in nearby supernova remnants suggests in situ dust formation, while other observations reveal very little dust in supernovae in the first few years after explosion. Observations of the spectral evolution of the bright SN 2010jl have been interpreted as pre-existing dust, dust formation or no dust at all. Here we report the rapid (40 to 240 days) formation of dust in its dense circumstellar medium. The wavelength-dependent extinction of this dust reveals the presence of very large (exceeding one micrometre) grains, which resist destruction. At later times (500 to 900 days), the near-infrared thermal emission shows an accelerated growth in dust mass, marking the transition of the dust source from the circumstellar medium to the ejecta. This provides the link between the early and late dust mass evolution in supernovae with dense circumstellar media.
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15
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Affiliation(s)
- Haley Gomez
- School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
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Metallofullerene and fullerene formation from condensing carbon gas under conditions of stellar outflows and implication to stardust. Proc Natl Acad Sci U S A 2013; 110:18081-6. [PMID: 24145444 DOI: 10.1073/pnas.1315928110] [Citation(s) in RCA: 45] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Carbonaceous presolar grains of supernovae origin have long been isolated and are determined to be the carrier of anomalous (22)Ne in ancient meteorites. That exotic (22)Ne is, in fact, the decay isotope of relatively short-lived (22)Na formed by explosive nucleosynthesis, and therefore, a selective and rapid Na physical trapping mechanism must take place during carbon condensation in supernova ejecta. Elucidation of the processes that trap Na and produce large carbon molecules should yield insight into carbon stardust enrichment and formation. Herein, we demonstrate that Na effectively nucleates formation of Na@C60 and other metallofullerenes during carbon condensation under highly energetic conditions in oxygen- and hydrogen-rich environments. Thus, fundamental carbon chemistry that leads to trapping of Na is revealed, and should be directly applicable to gas-phase chemistry involving stellar environments, such as supernova ejecta. The results indicate that, in addition to empty fullerenes, metallofullerenes should be constituents of stellar/circumstellar and interstellar space. In addition, gas-phase reactions of fullerenes with polycyclic aromatic hydrocarbons are investigated to probe "build-up" and formation of carbon stardust, and provide insight into fullerene astrochemistry.
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Goumans TPM, Bromley ST. Stardust silicate nucleation kick-started by SiO+TiO₂. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2013; 371:20110580. [PMID: 23734047 DOI: 10.1098/rsta.2011.0580] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
Dust particles are quintessential for the chemical evolution of the Universe. Dust nucleates in stellar outflows of dying stars and subsequently travels through the interstellar medium, continuously evolving via energetic processing, collisions and condensation. Finally, dust particles are incorporated in the next-generation star or its surrounding planetary system. In oxygen-rich stellar outflows, silicates are observed in the condensation zone (1200-1000 K), but, in spite of several decades of experimental and theoretical study, the stardust nucleation process remains poorly understood. We have previously shown that under these conditions ternary Mg-Si-O clusters may start forming at high enough rates from SiO, Mg and H₂O through heteromolecular association processes. In this reaction scheme, none of the possible initial association reactions was thermodynamically favourable owing to the large entropy loss at these temperatures. Here, we follow a previous idea that the incorporation of TiO₂ could help to initiate stardust nucleation. In contrast to these studies, we find that there is no need for TiO₂ cluster seeds-instead, one molecule of TiO₂ is sufficient to kick-start the subsequent nucleation of a silicate dust particle.
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Affiliation(s)
- T P M Goumans
- Gorlaeus Laboratories, Leiden Institute of Chemistry, Leiden University, PO Box 9502, Leiden 2300 RA, The Netherlands.
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Abstract
A source of interstellar dust that plays a crucial role in the formation of stars and the evolution of galaxies may have been discovered.
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Affiliation(s)
- Christopher F McKee
- Department of Physics, University of California at Berkeley, Berkeley, CA 94720, USA.
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19
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Matson J. Supernovae seed galaxies with massive amounts of dust. Nature 2011. [DOI: 10.1038/news.2011.404] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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