Dynamical simulations of HD 69830

Matthew J. Payne, Eric B. Ford, Mark C. Wyatt, Mark Booth

Research output: Contribution to journalArticle

Abstract

Previous studies have developed models for the growth and migration of three planets orbiting HD 69830. We perform n-body simulations using MERCURY (Chambers 1999) to explore the implications of these models for: 1) the excitation of planetary orbits via planet-planet interactions, 2) the accretion and clearing of a putative planetesimal disk, 3) the distribution of planetesimal orbits following migration, and 4) the implications for the origin of the observed infrared emission from the HD 69830 system. We report preliminary results that suggest new constraints on the formation of HD 69830.

Original languageEnglish (US)
Pages (from-to)540-543
Number of pages4
JournalProceedings of the International Astronomical Union
Volume4
Issue numberS253
DOIs
StatePublished - May 1 2008

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planets
protoplanets
planet
planetesimal
planetary orbits
simulation
clearing
chambers
accretion
orbits
excitation
interactions
distribution

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics

Cite this

Payne, Matthew J. ; Ford, Eric B. ; Wyatt, Mark C. ; Booth, Mark. / Dynamical simulations of HD 69830. In: Proceedings of the International Astronomical Union. 2008 ; Vol. 4, No. S253. pp. 540-543.
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Dynamical simulations of HD 69830. / Payne, Matthew J.; Ford, Eric B.; Wyatt, Mark C.; Booth, Mark.

In: Proceedings of the International Astronomical Union, Vol. 4, No. S253, 01.05.2008, p. 540-543.

Research output: Contribution to journalArticle

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