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Burkhardt C, Spitzer F, Morbidelli A, Budde G, Render JH, Kruijer TS, Kleine T. Terrestrial planet formation from lost inner solar system material. SCIENCE ADVANCES 2021; 7:eabj7601. [PMID: 34936445 PMCID: PMC8694615 DOI: 10.1126/sciadv.abj7601] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/31/2021] [Accepted: 11/03/2021] [Indexed: 06/14/2023]
Abstract
Two fundamentally different processes of rocky planet formation exist, but it is unclear which one built the terrestrial planets of the solar system. They formed either by collisions among planetary embryos from the inner solar system or by accreting sunward-drifting millimeter-sized “pebbles” from the outer solar system. We show that the isotopic compositions of Earth and Mars are governed by two-component mixing among inner solar system materials, including material from the innermost disk unsampled by meteorites, whereas the contribution of outer solar system material is limited to a few percent by mass. This refutes a pebble accretion origin of the terrestrial planets but is consistent with collisional growth from inner solar system embryos. The low fraction of outer solar system material in Earth and Mars indicates the presence of a persistent dust-drift barrier in the disk, highlighting the specific pathway of rocky planet formation in the solar system.
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Affiliation(s)
- Christoph Burkhardt
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| | - Fridolin Spitzer
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| | - Alessandro Morbidelli
- Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, Boulevard de l’Observatoire, 06304 Nice, Cedex 4, France
| | - Gerrit Budde
- Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA
| | - Jan H. Render
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| | - Thomas S. Kruijer
- Museum für Naturkunde, Leibniz Institute for Evolution and Biodiversity Science, Invalidenstraße 43, 10115 Berlin, Germany
- Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstraße 74-100, 12249 Berlin, Germany
| | - Thorsten Kleine
- Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
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Newborn stars don’t have enough dust to build planets. What are the missing ingredients? Proc Natl Acad Sci U S A 2019; 116:7605-7607. [DOI: 10.1073/pnas.1904572116] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
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Raymond SN, Izidoro A. The empty primordial asteroid belt. SCIENCE ADVANCES 2017; 3:e1701138. [PMID: 28924609 PMCID: PMC5597311 DOI: 10.1126/sciadv.1701138] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/11/2017] [Accepted: 08/14/2017] [Indexed: 05/23/2023]
Abstract
The asteroid belt contains less than a thousandth of Earth's mass and is radially segregated, with S-types dominating the inner belt and C-types the outer belt. It is generally assumed that the belt formed with far more mass and was later strongly depleted. We show that the present-day asteroid belt is consistent with having formed empty, without any planetesimals between Mars and Jupiter's present-day orbits. This is consistent with models in which drifting dust is concentrated into an isolated annulus of terrestrial planetesimals. Gravitational scattering during terrestrial planet formation causes radial spreading, transporting planetesimals from inside 1 to 1.5 astronomical units out to the belt. Several times the total current mass in S-types is implanted, with a preference for the inner main belt. C-types are implanted from the outside, as the giant planets' gas accretion destabilizes nearby planetesimals and injects a fraction into the asteroid belt, preferentially in the outer main belt. These implantation mechanisms are simple by-products of terrestrial and giant planet formation. The asteroid belt may thus represent a repository for planetary leftovers that accreted across the solar system but not in the belt itself.
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Affiliation(s)
- Sean N. Raymond
- Laboratoire d’Astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, 33615 Pessac, France
| | - Andre Izidoro
- Laboratoire d’Astrophysique de Bordeaux, Université de Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, 33615 Pessac, France
- Universidade Estadual Paulista (UNESP), Grupo de Dinamica Orbital e Planetologia, Guaratinguetá, CEP 12.516-410, São Paulo, Brazil
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Meech KJ. Setting the scene: what did we know before Rosetta? PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2017; 375:rsta.2016.0247. [PMID: 28554969 PMCID: PMC5454221 DOI: 10.1098/rsta.2016.0247] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 03/06/2017] [Indexed: 05/25/2023]
Abstract
This paper provides an overview of our state of knowledge about comets prior to the Rosetta mission encounter. Starting with the historical perspective, this paper discusses the development of comet science up to the modern era of space exploration. The extent to which comets are tracers of solar system formation processes or preserve pristine interstellar material has been investigated for over four decades. There is increasing evidence that in contrast with the distinct dynamical comet reservoirs we see today, comet formation regions strongly overlapped in the protoplanetary disc and there was significant migration of material in the disc during the epoch of comet formation. Comet nuclei are now known to be very low-density highly porous bodies, with very low thermal inertia, and have a range of sizes which exhibit a deficiency of very small bodies. The low thermal inertia suggests that comets may preserve pristine materials close to the surface, and that this might be accessible to sample return missions.This article is part of the themed issue 'Cometary science after Rosetta'.
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Affiliation(s)
- K J Meech
- Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
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Age of Jupiter inferred from the distinct genetics and formation times of meteorites. Proc Natl Acad Sci U S A 2017; 114:6712-6716. [PMID: 28607079 DOI: 10.1073/pnas.1704461114] [Citation(s) in RCA: 244] [Impact Index Per Article: 34.9] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The age of Jupiter, the largest planet in our Solar System, is still unknown. Gas-giant planet formation likely involved the growth of large solid cores, followed by the accumulation of gas onto these cores. Thus, the gas-giant cores must have formed before dissipation of the solar nebula, which likely occurred within less than 10 My after Solar System formation. Although such rapid accretion of the gas-giant cores has successfully been modeled, until now it has not been possible to date their formation. Here, using molybdenum and tungsten isotope measurements on iron meteorites, we demonstrate that meteorites derive from two genetically distinct nebular reservoirs that coexisted and remained spatially separated between ∼1 My and ∼3-4 My after Solar System formation. The most plausible mechanism for this efficient separation is the formation of Jupiter, opening a gap in the disk and preventing the exchange of material between the two reservoirs. As such, our results indicate that Jupiter's core grew to ∼20 Earth masses within <1 My, followed by a more protracted growth to ∼50 Earth masses until at least ∼3-4 My after Solar System formation. Thus, Jupiter is the oldest planet of the Solar System, and its solid core formed well before the solar nebula gas dissipated, consistent with the core accretion model for giant planet formation.
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Shinbrot T, Sabuwala T, Siu T, Vivar Lazo M, Chakraborty P. Size Sorting on the Rubble-Pile Asteroid Itokawa. PHYSICAL REVIEW LETTERS 2017; 118:111101. [PMID: 28368621 DOI: 10.1103/physrevlett.118.111101] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/02/2016] [Indexed: 06/07/2023]
Abstract
Photographs of the asteroid Itokawa reveal unexpectedly strong size segregation between lowlands populated almost entirely by small pebbles and highlands consisting of larger boulders. We propose that this segregation may be caused by a simple and unexplored effect: pebbles accreting onto the asteroid rebound from boulders, but sink into pebbly regions. By number, overwhelmingly more particles on Itokawa are pebbles, and collisions involving these pebbles must unavoidably cause pebbly regions to grow. We carry out experiments and simulations that demonstrate that this mechanism of size sorting based on simple counting of grains produces strong lateral segregation that reliably obeys an analytic formula.
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Affiliation(s)
- Troy Shinbrot
- Physics Department, Rutgers University, Piscataway, New Jersey 08854, USA
| | - Tapan Sabuwala
- Continuum Physics Unit, Okinawa Institute of Science and Technology, Onna-son, Okinawa 904-0495, Japan
| | - Theo Siu
- Physics Department, Rutgers University, Piscataway, New Jersey 08854, USA
| | - Miguel Vivar Lazo
- Physics Department, Rutgers University, Piscataway, New Jersey 08854, USA
| | - Pinaki Chakraborty
- Fluid Mechanics Unit, Okinawa Institute of Science and Technology, Onna-son, Okinawa 904-0495, Japan
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Johnson BC, Walsh KJ, Minton DA, Krot AN, Levison HF. Timing of the formation and migration of giant planets as constrained by CB chondrites. SCIENCE ADVANCES 2016; 2:e1601658. [PMID: 27957541 PMCID: PMC5148210 DOI: 10.1126/sciadv.1601658] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/19/2016] [Accepted: 11/08/2016] [Indexed: 05/23/2023]
Abstract
The presence, formation, and migration of giant planets fundamentally shape planetary systems. However, the timing of the formation and migration of giant planets in our solar system remains largely unconstrained. Simulating planetary accretion, we find that giant planet migration produces a relatively short-lived spike in impact velocities lasting ~0.5 My. These high-impact velocities are required to vaporize a significant fraction of Fe,Ni metal and silicates and produce the CB (Bencubbin-like) metal-rich carbonaceous chondrites, a unique class of meteorites that were created in an impact vapor-melt plume ~5 My after the first solar system solids. This indicates that the region where the CB chondrites formed was dynamically excited at this early time by the direct interference of the giant planets. Furthermore, this suggests that the formation of the giant planet cores was protracted and the solar nebula persisted until ~5 My.
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Affiliation(s)
- Brandon C. Johnson
- Department of Earth, Environmental and Planetary Sciences, Brown University, 324 Brook Street, Providence, RI 02912, USA
| | - Kevin J. Walsh
- Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
| | - David A. Minton
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, 550 Stadium Mall Drive, West Lafayette, IN 47907, USA
| | - Alexander N. Krot
- Hawai‘i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai‘i at Mānoa, 1680 East-West Road, Honolulu, HI 96822, USA
| | - Harold F. Levison
- Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
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The Mars anomaly. Proc Natl Acad Sci U S A 2016; 113:3704-7. [DOI: 10.1073/pnas.1603150113] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
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Meech KJ, Yang B, Kleyna J, Hainaut OR, Berdyugina S, Keane JV, Micheli M, Morbidelli A, Wainscoat RJ. Inner solar system material discovered in the Oort cloud. SCIENCE ADVANCES 2016; 2:e1600038. [PMID: 27386512 PMCID: PMC4928888 DOI: 10.1126/sciadv.1600038] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/08/2016] [Accepted: 03/30/2016] [Indexed: 05/31/2023]
Abstract
We have observed C/2014 S3 (PANSTARRS), a recently discovered object on a cometary orbit coming from the Oort cloud that is physically similar to an inner main belt rocky S-type asteroid. Recent dynamical models successfully reproduce the key characteristics of our current solar system; some of these models require significant migration of the giant planets, whereas others do not. These models provide different predictions on the presence of rocky material expelled from the inner solar system in the Oort cloud. C/2014 S3 could be the key to verifying these predictions of the migration-based dynamical models. Furthermore, this object displays a very faint, weak level of comet-like activity, five to six orders of magnitude less than that of typical ice-rich comets on similar Orbits coming from the Oort cloud. For the nearly tailless appearance, we are calling C/2014 S3 a Manx object. Various arguments convince us that this activity is produced by sublimation of volatile ice, that is, normal cometary activity. The activity implies that C/2014 S3 has retained a tiny fraction of the water that is expected to be present at its formation distance in the inner solar system. We may be looking at fresh inner solar system Earth-forming material that was ejected from the inner solar system and preserved for billions of years in the Oort cloud.
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Affiliation(s)
- Karen J. Meech
- Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822–1839, USA
| | - Bin Yang
- European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago, Chile
| | - Jan Kleyna
- Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822–1839, USA
| | - Olivier R. Hainaut
- European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
| | - Svetlana Berdyugina
- Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822–1839, USA
- Kiepenheuer Institut fuer Sonnenphysik, Schoeneckstrasse 6, 79104 Freiburg, Germany
| | - Jacqueline V. Keane
- Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822–1839, USA
| | - Marco Micheli
- Space Situational Awareness (SSA)–Near Earth Objects (NEO) Coordination Centre, European Space Agency, 00044 Frascati (RM), Italy
- SpaceDyS s.r.l., 56023 Cascina (Pl), Italy
- Istituto Nazionale di Astrofisica (INAF)–Istituto di Astrofisica e Planetologia Spaziali (IAPS), 00133 Roma (RM), Italy
| | - Alessandro Morbidelli
- Laboratoire Lagrange, UMR 7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Cöte d’Azur, Boulevard de l’Observatoire, 06304 Nice Cedex 4, France
| | - Richard J. Wainscoat
- Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822–1839, USA
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Growing the terrestrial planets from the gradual accumulation of submeter-sized objects. Proc Natl Acad Sci U S A 2015; 112:14180-5. [PMID: 26512109 DOI: 10.1073/pnas.1513364112] [Citation(s) in RCA: 123] [Impact Index Per Article: 13.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Building the terrestrial planets has been a challenge for planet formation models. In particular, classical theories have been unable to reproduce the small mass of Mars and instead predict that a planet near 1.5 astronomical units (AU) should roughly be the same mass as Earth. Recently, a new model called Viscously Stirred Pebble Accretion (VSPA) has been developed that can explain the formation of the gas giants. This model envisions that the cores of the giant planets formed from 100- to 1,000-km bodies that directly accreted a population of pebbles-submeter-sized objects that slowly grew in the protoplanetary disk. Here we apply this model to the terrestrial planet region and find that it can reproduce the basic structure of the inner solar system, including a small Mars and a low-mass asteroid belt. Our models show that for an initial population of planetesimals with sizes similar to those of the main belt asteroids, VSPA becomes inefficient beyond ∼ 1.5 AU. As a result, Mars's growth is stunted, and nothing large in the asteroid belt can accumulate.
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Witze A. Small rocks build big planets. Nature 2015. [DOI: 10.1038/nature.2015.18200] [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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