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Title: MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK

Abstract

Planetary migration poses a serious challenge to theories of planet formation. In gaseous and planetesimal disks, migration can remove planets as quickly as they form. To explore migration in a planetesimal disk, we combine analytic and numerical approaches. After deriving general analytic migration rates for isolated planets, we use N-body simulations to confirm these results for fast and slow migration modes. Migration rates scale as m{sup -1} (for massive planets) and (1 + (e{sub H}/3){sup 3}){sup -1}, where m is the mass of a planet and e{sub H} is the eccentricity of the background planetesimals in Hill units. When multiple planets stir the disk, our simulations yield the new result that large-scale migration ceases. Thus, growing planets do not migrate through planetesimal disks. To extend these results to migration in gaseous disks, we compare physical interactions and rates. Although migration through a gaseous disk is an important issue for the formation of gas giants, we conclude that migration has little impact on the formation of terrestrial planets.

Authors:
 [1]
  1. Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Rm 201, Salt Lake City, UT 84112 (United States)
Publication Date:
OSTI Identifier:
21576569
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 735; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/735/1/29; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; MIGRATION; PLANETS; SIMULATION

Citation Formats

Bromley, Benjamin C, and Kenyon, Scott J., E-mail: bromley@physics.utah.edu, E-mail: skenyon@cfa.harvard.edu. MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK. United States: N. p., 2011. Web. doi:10.1088/0004-637X/735/1/29.
Bromley, Benjamin C, & Kenyon, Scott J., E-mail: bromley@physics.utah.edu, E-mail: skenyon@cfa.harvard.edu. MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK. United States. https://doi.org/10.1088/0004-637X/735/1/29
Bromley, Benjamin C, and Kenyon, Scott J., E-mail: bromley@physics.utah.edu, E-mail: skenyon@cfa.harvard.edu. 2011. "MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK". United States. https://doi.org/10.1088/0004-637X/735/1/29.
@article{osti_21576569,
title = {MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK},
author = {Bromley, Benjamin C and Kenyon, Scott J., E-mail: bromley@physics.utah.edu, E-mail: skenyon@cfa.harvard.edu},
abstractNote = {Planetary migration poses a serious challenge to theories of planet formation. In gaseous and planetesimal disks, migration can remove planets as quickly as they form. To explore migration in a planetesimal disk, we combine analytic and numerical approaches. After deriving general analytic migration rates for isolated planets, we use N-body simulations to confirm these results for fast and slow migration modes. Migration rates scale as m{sup -1} (for massive planets) and (1 + (e{sub H}/3){sup 3}){sup -1}, where m is the mass of a planet and e{sub H} is the eccentricity of the background planetesimals in Hill units. When multiple planets stir the disk, our simulations yield the new result that large-scale migration ceases. Thus, growing planets do not migrate through planetesimal disks. To extend these results to migration in gaseous disks, we compare physical interactions and rates. Although migration through a gaseous disk is an important issue for the formation of gas giants, we conclude that migration has little impact on the formation of terrestrial planets.},
doi = {10.1088/0004-637X/735/1/29},
url = {https://www.osti.gov/biblio/21576569}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 735,
place = {United States},
year = {Fri Jul 01 00:00:00 EDT 2011},
month = {Fri Jul 01 00:00:00 EDT 2011}
}