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Formation of Comets. UNIVERSE 2022. [DOI: 10.3390/universe8070381] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/04/2022]
Abstract
Questions regarding how primordial or pristine the comets of the solar system are have been an ongoing controversy. In this review, we describe comets’ physical evolution from dust and ice grains in the solar nebula to the contemporary small bodies in the outer solar system. This includes the phases of dust agglomeration, the formation of planetesimals, their thermal evolution and the outcomes of collisional processes. We use empirical evidence about comets, in particular from the Rosetta Mission to comet 67P/Churyumov–Gerasimenko, to draw conclusions about the possible thermal and collisional evolution of comets.
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Manser CJ, Gänsicke BT, Eggl S, Hollands M, Izquierdo P, Koester D, Landstreet JD, Lyra W, Marsh TR, Meru F, Mustill AJ, Rodríguez-Gil P, Toloza O, Veras D, Wilson DJ, Burleigh MR, Davies MB, Farihi J, Gentile Fusillo N, de Martino D, Parsons SG, Quirrenbach A, Raddi R, Reffert S, Del Santo M, Schreiber MR, Silvotti R, Toonen S, Villaver E, Wyatt M, Xu S, Portegies Zwart S. A planetesimal orbiting within the debris disc around a white dwarf star. Science 2019; 364:66-69. [PMID: 30948547 DOI: 10.1126/science.aat5330] [Citation(s) in RCA: 115] [Impact Index Per Article: 23.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/09/2018] [Accepted: 02/26/2019] [Indexed: 12/30/2022]
Abstract
Many white dwarf stars show signs of having accreted smaller bodies, implying that they may host planetary systems. A small number of these systems contain gaseous debris discs, visible through emission lines. We report a stable 123.4-minute periodic variation in the strength and shape of the Ca ii emission line profiles originating from the debris disc around the white dwarf SDSS J122859.93+104032.9. We interpret this short-period signal as the signature of a solid-body planetesimal held together by its internal strength.
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Affiliation(s)
| | - Boris T Gänsicke
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK.,Centre for Exoplanets and Habitability, University of Warwick, Coventry CV4 7AL, UK
| | - Siegfried Eggl
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - Mark Hollands
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - Paula Izquierdo
- Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain.,Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - Detlev Koester
- Institut für Theoretische Physik und Astrophysik, Universität Kiel, 24098 Kiel, Germany
| | - John D Landstreet
- Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, N6A 3K7, Canada.,Armagh Observatory and Planetarium, College Hill, Armagh, Co. Armagh BT61 9DG, UK
| | - Wladimir Lyra
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.,Department of Physics and Astronomy, California State University, Northridge, 18111 Nordhoff St., Northridge, CA 91330, USA
| | - Thomas R Marsh
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - Farzana Meru
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - Alexander J Mustill
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, SE-221 00 Lund, Sweden
| | - Pablo Rodríguez-Gil
- Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain.,Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - Odette Toloza
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - Dimitri Veras
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK.,Centre for Exoplanets and Habitability, University of Warwick, Coventry CV4 7AL, UK
| | - David J Wilson
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK.,McDonald Observatory, University of Texas at Austin, Austin, TX 78712, USA
| | - Matthew R Burleigh
- Department of Physics and Astronomy, Leicester Institute of Space and Earth Observation, University of Leicester, University Road, Leicester LE1 7RH, UK
| | - Melvyn B Davies
- Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, SE-221 00 Lund, Sweden
| | - Jay Farihi
- Physics and Astronomy, University College London, London WC1E 6BT, UK
| | | | - Domitilla de Martino
- Osservatorio Astronomico di Capodimonte, National Institute for Astrophysics, Via Moiarello 16, 80131 Napoli, Italy
| | - Steven G Parsons
- Department of Physics and Astronomy, The University of Sheffield, Western Bank, Sheffield S10 2TN, UK
| | - Andreas Quirrenbach
- Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany
| | - Roberto Raddi
- Dr. Karl Remeis-Sternwarte, Astronomisches Institut der Universität Erlangen-Nürnberg, Sternwartestr. 7, 96049, Bamberg, Germany
| | - Sabine Reffert
- Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany
| | - Melania Del Santo
- National Institute for Astrophysics/Institute of Space Astrophysics and Cosmic Physics, via Ugo La Malfa 153, 90146, Palermo, Italy
| | - Matthias R Schreiber
- Instituto de Física y Astronomía, Universidad de Valparaíso, Av. Gran Bretaña 1111, 5030 Casilla, Valparaíso, Chile.,Milennium Nucleus for Planet Formation - NPF, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile
| | - Roberto Silvotti
- National Institute for Astrophysics, Osservatorio Astrofisico di Torino, Strada dell'Osservatorio 20, 10025 Pino Torinese, Italy
| | - Silvia Toonen
- Anton Pannekoek Instituut voor Sterrenkunde, University of Amsterdam, P.O. Box 94249, 1090 GE, Amsterdam, Netherlands
| | - Eva Villaver
- Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco 28049 Madrid, Spain
| | - Mark Wyatt
- Institute of Astronomy, Madingley Rd, Cambridge CB3 0HA, UK
| | - Siyi Xu
- Gemini Observatory, Northern Operations Center, 670 N. A'ohoku Place, Hilo, HI 96720, USA
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High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/aaf389] [Citation(s) in RCA: 37] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aaf740] [Citation(s) in RCA: 243] [Impact Index Per Article: 40.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aaf741] [Citation(s) in RCA: 524] [Impact Index Per Article: 87.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Identifying Anticyclonic Vortex Features Produced by the Rossby Wave Instability in Protoplanetary Disks. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aae317] [Citation(s) in RCA: 21] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Dust-trapping Vortices and a Potentially Planet-triggered Spiral Wake in the Pre-transitional Disk of V1247 Orionis. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/2041-8213/aa8edc] [Citation(s) in RCA: 49] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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9
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A Resolved and Asymmetric Ring of PAHs within the Young Circumstellar Disk of IRS 48. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/aa74b7] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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10
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Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-3881/aa6d85] [Citation(s) in RCA: 83] [Impact Index Per Article: 11.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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11
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An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-3881/aa6cae] [Citation(s) in RCA: 66] [Impact Index Per Article: 9.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Polycyclic Aromatic Hydrocarbons in Protoplanetary Disks around Herbig Ae/Be and T Tauri Stars. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/835/2/291] [Citation(s) in RCA: 39] [Impact Index Per Article: 5.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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DUST CAPTURE AND LONG-LIVED DENSITY ENHANCEMENTS TRIGGERED BY VORTICES IN 2D PROTOPLANETARY DISKS. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/831/1/82] [Citation(s) in RCA: 54] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Pacheco-Vázquez S, Fuente A, Baruteau C, Berné O, Agúndez M, Neri R, Goicoechea JR, Cernicharo J, Bachiller R. High spatial resolution imaging of SO and H 2CO in AB Auriga: The first SO image in a transitional disk. ASTRONOMY AND ASTROPHYSICS 2016; 589:A60. [PMID: 27279654 PMCID: PMC4894459 DOI: 10.1051/0004-6361/201527089] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
CONTEXT Transitional disks are structures of dust and gas around young stars with large inner cavities in which planet formation may occur. Lopsided dust distributions are observed in the dust continuum emission at millimeter wavelengths. These asymmetrical structures can be explained as being the result of an enhanced gas density vortex where the dust is trapped, potentially promoting the rapid growth to the planetesimal scale. AIMS AB Aur hosts a transitional disk with a clear horseshoe morphology which strongly suggests the presence of a dust trap. Our goal is to investigate its formation and the possible effects on the gas chemistry. METHODS We used the NOEMA (NOrthern Extended Millimeter Array) interferometer to image the 1mm continuum dust emission and the 13CO J=2 →1, C18OJ=2 →1, SO J=56 →45, and H2CO J=303 →202 rotational lines. RESULTS Line integrated intensity ratio images are built to investigate the chemical changes within the disk. The I(H2CO J=303 →202)/I(C18O J=2→1) ratio is fairly constant along the disk with values of ~0.15±0.05. On the contrary, the I(SO J=56 →45)/I(C18O J=2 →1) and I(SO J=56 →45)/I(H2CO J=303 →202) ratios present a clear northeast-southwest gradient (a factor of 3-6) with the minimum towards the dust trap. This gradient cannot be explained by a local change in the excitation conditions but by a decrease in the SO abundance. Gas densities up to ~109 cm-3 are expected in the disk midplane and two-three times larger in the high pressure vortex. We have used a single point (n,T) chemical model to investigate the lifetime of gaseous CO, H2CO, and SO in the dust trap. Our model shows that for densities >107 cm-3, the SO molecules are depleted (directly frozen, or converted into SO2 and then frozen out) in less than 0.1 Myr. The lower SO abundance towards the dust trap could indicate that a larger fraction of the gas is in a high density environment. CONCLUSIONS Gas dynamics, grain growth and gas chemistry are coupled in the planet formation process. We detect a chemical signature of the presence of a dust trap in a transitional disk. Because of the strong dependence of SO abundance on the gas density, the sulfur chemistry can be used as a chemical diagnostic to detect the birthsites of future planets. However, the large uncertainties inherent to chemical models and the limited knowledge of the disk's physical structure and initial conditions are important drawbacks.
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Affiliation(s)
- S Pacheco-Vázquez
- Observatorio Astronómico Nacional (OAN), Apdo 112, E-28803 Alcalá de Henares, Madrid, Spain ,
| | - A Fuente
- Observatorio Astronómico Nacional (OAN), Apdo 112, E-28803 Alcalá de Henares, Madrid, Spain ,
| | - C Baruteau
- CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - O Berné
- CNRS, IRAP, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France; Université de Toulouse, UPS-OMP, IRAP, Toulouse, France
| | - M Agúndez
- Instituto de Ciencia de Materiales de Madrid, ICMM-CSIC, C/ Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Spain
| | - R Neri
- Institut de Radioastronomie Millimétrique, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France
| | - J R Goicoechea
- Instituto de Ciencia de Materiales de Madrid, ICMM-CSIC, C/ Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Spain
| | - J Cernicharo
- Instituto de Ciencia de Materiales de Madrid, ICMM-CSIC, C/ Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Spain
| | - R Bachiller
- Observatorio Astronómico Nacional (OAN), Apdo 112, E-28803 Alcalá de Henares, Madrid, Spain ,
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Casassus S, Wright CM, Marino S, Maddison ST, Wootten A, Roman P, Pérez S, Pinilla P, Wyatt M, Moral V, Ménard F, Christiaens V, Cieza L, Plas GVD. A COMPACT CONCENTRATION OF LARGE GRAINS IN THE HD 142527 PROTOPLANETARY DUST TRAP. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/812/2/126] [Citation(s) in RCA: 102] [Impact Index Per Article: 11.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Batygin K, Laughlin G. Jupiter's decisive role in the inner Solar System's early evolution. Proc Natl Acad Sci U S A 2015; 112:4214-7. [PMID: 25831540 PMCID: PMC4394287 DOI: 10.1073/pnas.1423252112] [Citation(s) in RCA: 88] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The statistics of extrasolar planetary systems indicate that the default mode of planet formation generates planets with orbital periods shorter than 100 days and masses substantially exceeding that of the Earth. When viewed in this context, the Solar System is unusual. Here, we present simulations which show that a popular formation scenario for Jupiter and Saturn, in which Jupiter migrates inward from a > 5 astronomical units (AU) to a ≈ 1.5 AU before reversing direction, can explain the low overall mass of the Solar System's terrestrial planets, as well as the absence of planets with a < 0.4 AU. Jupiter's inward migration entrained s ≳ 10-100 km planetesimals into low-order mean motion resonances, shepherding and exciting their orbits. The resulting collisional cascade generated a planetesimal disk that, evolving under gas drag, would have driven any preexisting short-period planets into the Sun. In this scenario, the Solar System's terrestrial planets formed from gas-starved mass-depleted debris that remained after the primary period of dynamical evolution.
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Affiliation(s)
- Konstantin Batygin
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125; and
| | - Greg Laughlin
- Department of Astronomy & Astrophysics, University of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064
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Dutrey A, Di Folco E, Guilloteau S, Boehler Y, Bary J, Beck T, Beust H, Chapillon E, Gueth F, Huré JM, Pierens A, Piétu V, Simon M, Tang YW. Possible planet formation in the young, low-mass, multiple stellar system GG Tau A. Nature 2014; 514:600-2. [PMID: 25355359 DOI: 10.1038/nature13822] [Citation(s) in RCA: 46] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/19/2014] [Accepted: 09/01/2014] [Indexed: 11/09/2022]
Abstract
The formation of planets around binary stars may be more difficult than around single stars. In a close binary star (with a separation of less than a hundred astronomical units), theory predicts the presence of circumstellar disks around each star, and an outer circumbinary disk surrounding a gravitationally cleared inner cavity around the stars. Given that the inner disks are depleted by accretion onto the stars on timescales of a few thousand years, any replenishing material must be transferred from the outer reservoir to fuel planet formation (which occurs on timescales of about one million years). Gas flowing through disk cavities has been detected in single star systems. A circumbinary disk was discovered around the young low-mass binary system GG Tau A (ref. 7), which has recently been shown to be a hierarchical triple system. It has one large inner disk around the single star, GG Tau Aa, and shows small amounts of shocked hydrogen gas residing within the central cavity, but other than a single weak detection, the distribution of cold gas in this cavity or in any other binary or multiple star system has not hitherto been determined. Here we report imaging of gas fragments emitting radiation characteristic of carbon monoxide within the GG Tau A cavity. From the kinematics we conclude that the flow appears capable of sustaining the inner disk (around GG Tau Aa) beyond the accretion lifetime, leaving time for planet formation to occur there. These results show the complexity of planet formation around multiple stars and confirm the general picture predicted by numerical simulations.
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Affiliation(s)
- Anne Dutrey
- 1] Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac, France [2] Centre National de la Recherche Scientifique (CNRS), LAB, UMR 5804, F-33270 Floirac, France
| | - Emmanuel Di Folco
- 1] Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac, France [2] Centre National de la Recherche Scientifique (CNRS), LAB, UMR 5804, F-33270 Floirac, France
| | - Stéphane Guilloteau
- 1] Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac, France [2] Centre National de la Recherche Scientifique (CNRS), LAB, UMR 5804, F-33270 Floirac, France
| | - Yann Boehler
- Centro de Radioastronomia y Astrofisica (CRyA), University of Mexico, Apartado Postal 3-72, 58089 Morelia, Michoacan, Mexico
| | - Jeff Bary
- Department of Physics and Astronomy, Colgate University, 13 Oak Drive, Hamilton, New York 13346, USA
| | - Tracy Beck
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218, USA
| | - Hervé Beust
- Institut de Planetologie et d'Astrophysique de Grenoble (IPAG), UMR 5274, BP 53, F-38041 Grenoble Cedex 9, France
| | - Edwige Chapillon
- 1] Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac, France [2] Institut de RadioAstronomie Millimetrique (IRAM), 300 rue de la Piscine, F-38046 Saint Martin d'Hères, France
| | - Fredéric Gueth
- Institut de RadioAstronomie Millimetrique (IRAM), 300 rue de la Piscine, F-38046 Saint Martin d'Hères, France
| | - Jean-Marc Huré
- 1] Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac, France [2] Centre National de la Recherche Scientifique (CNRS), LAB, UMR 5804, F-33270 Floirac, France
| | - Arnaud Pierens
- 1] Université de Bordeaux, LAB, UMR 5804, F-33270 Floirac, France [2] Centre National de la Recherche Scientifique (CNRS), LAB, UMR 5804, F-33270 Floirac, France
| | - Vincent Piétu
- Institut de RadioAstronomie Millimetrique (IRAM), 300 rue de la Piscine, F-38046 Saint Martin d'Hères, France
| | - Michal Simon
- Stony Brook University, Stony Brook, New York 11794-3800, USA
| | - Ya-Wen Tang
- Academia Sinica Institute of Astronomy and Astrophysics, PO Box 23-141, Taipei 106, Taiwan
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Walsh C, Juhász A, Pinilla P, Harsono D, Mathews GS, Dent WRF, Hogerheijde MR, Birnstiel T, Meeus G, Nomura H, Aikawa Y, Millar TJ, Sandell G. ALMA HINTS AT THE PRESENCE OF TWO COMPANIONS IN THE DISK AROUND HD 100546. ACTA ACUST UNITED AC 2014. [DOI: 10.1088/2041-8205/791/1/l6] [Citation(s) in RCA: 106] [Impact Index Per Article: 10.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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van Dishoeck EF. Astrochemistry of dust, ice and gas: introduction and overview. Faraday Discuss 2014; 168:9-47. [DOI: 10.1039/c4fd00140k] [Citation(s) in RCA: 98] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
A brief introduction and overview of the astrochemistry of dust, ice and gas and their interplay is presented. The importance of basic chemical physics studies of critical reactions is illustrated through a number of recent examples. Such studies have also triggered new insight into chemistry, illustrating how astronomy and chemistry can enhance each other. Much of the chemistry in star- and planet-forming regions is now thought to be driven by gas–grain chemistry rather than pure gas-phase chemistry, and a critical discussion of the state of such models is given. Recent developments in studies of diffuse clouds and PDRs, cold dense clouds, hot cores, protoplanetary disks and exoplanetary atmospheres are summarized, both for simple and more complex molecules, with links to papers presented in this volume. In spite of many lingering uncertainties, the future of astrochemistry is bright: new observational facilities promise major advances in our understanding of the journey of gas, ice and dust from clouds to planets.
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Affiliation(s)
- Ewine F. van Dishoeck
- Leiden Observatory
- Leiden University
- 2300 RA Leiden, the Netherlands
- Max-Planck-Institute für Extraterrestrische Physik
- Garching, Germany
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Affiliation(s)
- Thomas Henning
- Max Planck Institute for Astronomy, Königstuhl
17, D-69117 Heidelberg, Germany
| | - Dmitry Semenov
- Max Planck Institute for Astronomy, Königstuhl
17, D-69117 Heidelberg, Germany
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Trap holds protoplanet dust. Nature 2013. [DOI: 10.1038/498141a] [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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Affiliation(s)
- Philip J. Armitage
- JILA, University of Colorado and National Institute of Standards and Technology, Boulder, CO 80309-0440, USA
- Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA
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