FORMATION OF THE TERRESTRIAL PLANETS FROM A NARROW ANNULUS
Open accessAbstract
We show that the assembly of the solar system terrestrial planets can be successfully modeled with all of the mass initially confined to a narrow annulus between 0.7 and 1.0 AU. With this configuration, analogs of Mercury and Mars often form from the collisional evolution of material diffusing out of the annulus under the scattering of the forming Earth and Venus analogs. The final systems also possess eccentricities and inclinations that match the observations, without recourse to dynamical friction from remnant small body populations. Finally, the characteristic assembly timescale for Earth analogs is rapid in this model and consistent with cosmochemical models based on the 182 Hf– 182 W isotopes. The agreement between this model and the observations suggests that terrestrial planet systems may also be formed in "planet traps," as has been proposed recently for the cores of giant planets in our solar system and others.
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One solution to the Mars low-mass problem is to truncate the disk of planetesimals that accrete to produce the terrestrial planets at 1 AU.
“One solution to this problem is to truncate the disk of planetesimals that accrete to produce the terrestrial planets at 1 AU (Hansen, 2009).”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Hansen, 2009
Cites
A 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 · see citing works
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 · see citing works
THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON
Jacobsen, S. B. (2005) · Annual Review of Earth and Planetary Sciences · doi:10.1146/annurev.earth.33.092203.122614 · Cited by 234 · see citing works
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Domagal-Goldman, S. D., Wright, K. E., Domagal-Goldman, S. D., Wright, K. E., Adamala, K., Arina de la Rubia, L., Bond, J., Dartnell, L. R., Goldman, A. D., Lynch, K., et al. (2016) · Astrobiology · doi:10.1089/ast.2015.1460 · Cited by 136 · see citing works
“One solution to this problem is to truncate the disk of planetesimals that accrete to produce the terrestrial planets at 1 AU (Hansen, 2009).”
- Authors
- Hansen, B. M. S.
- Affiliations
- University of California, Los Angeles (US)
- Corresponding author
- Hansen, Brad M. S.
- ORCID
- Hansen, Brad M. S.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2009-09-04
- Volume
- 703
- Issue
- 1
- Pages
- 1131-1140
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2170490486
- Cited by
- 317
- References
- 3
- Citations by year
- 2026: 10 · 2025: 17 · 2024: 17 · 2023: 15 · 2022: 16 · 2021: 24 · 2020: 34 · 2019: 24 · 2018: 28 · 2017: 15 · 2016: 23 · 2015: 24 · 2014: 22 · 2013: 17 · 2012: 11
- FWCI
- 4.88
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- AAS
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Keywords
- terrestrial planet formation, collisional evolution, Mars analog, Earth analogs, orbital eccentricity, orbital inclination, solar system formation, giant planet cores
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