Astrophysics, abstract
astro-ph/0404212

From: Sean Raymond [view email]

Date (v1): Fri, 9 Apr 2004 20:03:38 GMT (38kb)
Date (revised v2): Fri, 24 Feb 2006 16:44:11 GMT (57kb)
Date (revised v3): Mon, 15 May 2006 17:28:52 GMT (57kb)

Predicting Planets in Known Extra-Solar Planetary Systems III: Forming Terrestrial Planets

Authors: Sean N. Raymond (Colorado), Rory Barnes (Arizona), Nathan A. Kaib (Washington)

Comments: New coauthor Kaib -- ApJ, in press

Recent results have shown that many of the known extrasolar planetary systems contain regions which are stable for both Earth-mass and Saturn-mass planets. Here we simulate the formation of terrestrial planets in four planetary systems -- 55 Cancri, HD 38529, HD 37124, and HD 74156 -- under the assumption that these systems of giant planets are complete and that their orbits are well-determined. Assuming the giant planets formed and migrated quickly, then terrestrial planets may form from a second generation of planetesimals. In each case, Moon- to Mars-sized planetary embryos are placed in between the giant planets and evolved for 100 Myr. We find that planets form relatively easily in 55 Cnc, with masses up to 0.6 Earth masses and in some cases substantial water contents and orbits in the habitable zone. HD 38529 is likely to support an asteroid belt but no terrestrial planets of significant mass. No terrestrial planets form in HD 37124 and HD 74156, although in some cases 1-2 lone embryos survive for 100 Myr. If migration occurred later, depleting the planetesimal disk, then massive terrestrial planets are unlikely to form in any of these systems.

http://arxiv.org/abs/astro-ph/0404212