On the formation of terrestrial planets in hot-Jupiter systems
| dc.creator | Fogg, Martyn J. | |
| dc.creator | Nelson, Richard P. | |
| dc.date | 2006-10-11 | |
| dc.date.accessioned | 2026-07-07T11:42:38Z | |
| dc.date.available | 2026-07-07T11:42:38Z | |
| dc.description | We present a series of calculations aimed at examining how an inner system of planetesimals/protoplanets, undergoing terrestrial planet formation, evolves under the influence of a giant planet undergoing inward type II migration through the region bounded between 5 - 0.1 AU. We find that > 60% of the solids disk survives by being scattered by the giant planet into external orbits. Planetesimals are scattered outward almost as efficiently as protoplanets, resulting in the regeneration of a solids disk where dynamical friction is strong and terrestrial planet formation is able to resume. A simulation extended for a few Myr after the migration of the giant planet halted at 0.1 AU, resulted in an apparently stable planet of ~ 2 Earth masses forming in the habitable zone. Migration-induced mixing of volatile-rich material from beyond the `snowline' into the inner disk regions means that terrestrial planets that form there are likely to be water-rich. We predict that hot--Jupiter systems are likely to harbor water-rich terrestrial planets in their habitable zones. These planets may be detected by future planet search missions. | |
| dc.description | 18 pages, 13 figures. Higher resolution pdf available at http://www.users.globalnet.co.uk/~mfogg/fogg_nelson2.pdf | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0610314 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0610314 | |
| dc.identifier | Astron.Astrophys.461:1195-1208,2007 | |
| dc.identifier | doi:10.1051/0004-6361:20066171 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/200951 | |
| dc.subject | Astrophysics | |
| dc.title | On the formation of terrestrial planets in hot-Jupiter systems | |
| dc.type | text |