The DOI matches its Crossref record; 186 of the 186 references it cites were found in a registry or an index.
Debris disks as signposts of terrestrial planet formation
Open accessAbstract
There exists strong circumstantial evidence from their eccentric orbits that most of the known extra-solar planetary systems are the survivors of violent dynamical instabilities. Here we explore the effect of giant planet instabilities on the formation and survival of terrestrial planets. We numerically simulate the evolution of planetary systems around Sun-like stars that include three components: (i) an inner disk of planetesimals and planetary embryos; (ii) three giant planets at Jupiter-Saturn distances; and (iii) an outer disk of planetesimals comparable to estimates of the primitive Kuiper belt. We calculate the dust production and spectral energy distribution of each system by assuming that each planetesimal particle represents an ensemble of smaller bodies in collisional equilibrium. Our main result is a strong correlation between the evolution of the inner and outer parts of planetary systems, i.e. between the presence of terrestrial planets and debris disks. Strong giant planet instabilities – that produce very eccentric surviving planets – destroy all rocky material in the system, including fully-formed terrestrial planets if the instabilities occur late, and also destroy the icy planetesimal population. Stable or weakly unstable systems allow terrestrial planets to accrete in their inner regions and significant dust to be produced in their outer regions, detectable at mid-infrared wavelengths as debris disks. Stars older than ~100 Myr with bright cold dust emission (in particular at λ ~ 70 μm) signpost dynamically calm environments that were conducive to efficient terrestrial accretion. Such emission is present around ~16% of billion-year old Solar-type stars. Our simulations yield numerous secondary results: 1) the typical eccentricities of as-yet undetected terrestrial planets are ~0.1 but there exists a novel class of terrestrial planet system whose single planet undergoes large amplitude oscillations in orbital eccentricity and inclination; 2) by scaling our systems to match the observed semimajor axis distribution of giant exoplanets, we predict that terrestrial exoplanets in the same systems should be a few times more abundant at ~0.5 AU than giant or terrestrial exoplanets at 1 AU; 3) the Solar System appears to be unusual in terms of its combination of a rich terrestrial planet system and a low dust content. This may be explained by the weak, outward-directed instability that is thought to have caused the late heavy bombardment.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Claims other papers make about this one
Each is checked against this paper’s own text: does it say what the citing paper says it does?
In the citing paper
“while planet-planet scattering among gas giant planets is likely to produce a pulse of ejected planetesimals (Raymond et al. 2011;Marzari 2014)”
From Implications for Planetary System Formation from Interstellar Object 1I/2017 U1 (‘Oumuamua) (2017) · cites this paper as Raymond et al. 2011
In the citing paper
“and while systems with gas giants on stable orbits can eject planetesimals on longer timescales (Raymond et al. 2011;Barclay et al. 2017)”
From Implications for Planetary System Formation from Interstellar Object 1I/2017 U1 (‘Oumuamua) (2017) · cites this paper as Raymond et al. 2011
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Formation of the Giant Planets by Concurrent Accretion of Solids and Gas
Pollack, J. B., Hubickyj, O., Bodenheimer, P. H., Lissauer, J. J., Podolak, M., & Greenzweig, Y. (1996) · Icarus · doi:10.1006/icar.1996.0190 · Cited by 3,152
Secular perturbations of asteroids with high inclination and eccentricity
Kozai, Y. (1962) · The Astronomical Journal · doi:10.1086/108790 · Cited by 2,588
Habitable Zones around Main Sequence Stars
Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. (1993) · Icarus · doi:10.1006/icar.1993.1010 · Cited by 2,501 · cited 1×
“The terrestrial planet’s final mass is 0.72 M⊕ and its semimajor axis of 0.935 AU places it in the circumstellar habitable zone (Kasting et al. 1993; Selsis et al. 2007).”
BackgroundInfluentialA hybrid symplectic integrator that permits close encounters between massive bodies
Chambers, J. E. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02379.x · Cited by 1,820
Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets
Gomes, R., Levison, H. F., Tsiganis, K., & Morbidelli, A. (2005) · Nature · doi:10.1038/nature03676 · Cited by 1,737
Disk frequencies and lifetimes in Young clusters
Haisch, Jr., Lada, E. A., & Lada, C. J. (2001) · The Astrophysical Journal · doi:10.1086/320685 · Cited by 1,723
The Planet‐Metallicity Correlation
Fischer, D. A., & Valenti, J. A. (2005) · The Astrophysical Journal · doi:10.1086/428383 · Cited by 1,641
Origin of the orbital architecture of the giant planets of the Solar System
Tsiganis, K., Gomes, R., Morbidelli, A., & Levison, H. F. (2005) · Nature · doi:10.1038/nature03539 · Cited by 1,476
A low mass for Mars from Jupiter’s early gas-driven migration
Walsh, K. J., Morbidelli, A., Raymond, S. N., O'Brien, D. P., & Mandell, A. M. (2011) · Nature · doi:10.1038/nature10201 · Cited by 1,241
Self-citationCollisional model of asteroids and their debris
Dohnanyi, J. S. (1969) · Journal of Geophysical Research Atmospheres · doi:10.1029/jb074i010p02531 · Cited by 1,220
Research works printed but not linked: 4
- Armitage, P. J. 2011, ARA&A, in press
- Ford, E. B., Rasio, F. A., & Yu, K. 2003, in Scientific Frontiers in Research on Extrasolar Planets, ed. D. Deming, & S. Seager, ASP Conf. Ser., 294, 181
- Kennedy, 2010, MNRAS, 405, 1253
- Laskar, 1993, A&A, 270, 522
Cited by
Sorted by citations
Perryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/9781108304160 · Cited by 380
SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions
Ziegler, C., Tokovinin, A. A., Briceño, C. A., Mang, J. J., Law, N., & Mann, A. W. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab55e9 · Cited by 267
Formation of planetary systems by pebble accretion and migration: growth of gas giants
Bitsch, B., Izidoro, A., Johansen, A., Raymond, S. N., Morbidelli, A., Lambrechts, M., & Jacobson, S. A. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834489 · Cited by 195
Self-citationThe empty primordial asteroid belt
Raymond, S. N., & Izidoro, A. (2017) · Science Advances · doi:10.1126/sciadv.1701138 · Cited by 165
Self-citationThe Nature and Origins of Sub‐Neptune Size Planets
Bean, J. L., Raymond, S. N., & Owen, J. E. (2020) · Journal of Geophysical Research Planets · doi:10.1029/2020je006639 · Cited by 152
Self-citation
Metadata
- Authors
- Raymond, S. N., Armitage, P. J., Moro-Martín, A., Booth, M., Wyatt, M. C., Armstrong, J. C., Mandell, A. M., Selsis, F., & West, A. A.
- Affiliations
- Centre National de la Recherche Scientifique (FR)
- Joint Institute for Laboratory Astrophysics (US)
- University of Victoria (CA)
- University of Cambridge (GB)
- Weber State University (US)
- Goddard Space Flight Center (US)
- Boston University (US)
- Venue
- Astronomy & Astrophysics
- Publisher
- EDP Sciences
- Published
- 2011-05-12
- Volume
- 530
- Pages
- A62
- ISSN
- 0004-6361 (ISSN-L)
- 1432-0746
- OpenAlex
- W1964193027
- Cited by
- 194
- References
- 184
- Citations by year
- 2026: 2 · 2025: 5 · 2024: 6 · 2023: 4 · 2022: 4 · 2021: 7 · 2020: 13 · 2019: 12 · 2018: 41 · 2017: 11 · 2016: 12 · 2015: 15 · 2014: 13 · 2013: 20 · 2012: 15
- FWCI
- 9.52
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- HAL (submittedVersion)
- Oskar-Bordeaux (Universite de Bordeaux) (submittedVersion)
- Funders
- National Science Foundation (0807471)
- National Aeronautics and Space Administration (NNX07AH08G, NNX09AB90G)
- Purdue University
- Weber State University
- University of Washington
- Centre National de la Recherche Scientifique
- NASA Astrobiology Institute
- Science and Technology Facilities Council (ST/H00243X/1, ST/G00269X/1)
- Division of Astronomical Sciences
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Keywords
- debris disks, terrestrial planet formation, giant planet instability, dynamical instability, dust formation, mid-infrared dust emission, eccentric planets, terrestrial exoplanets, giant exoplanets, Kuiper belt analog, Late Heavy Bombardment, solar-type stars
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
