Dispersing the Gaseous Protoplanetary Disk and Halting Type II Migration | Zendy

M. Lecar | Zendy; Dimitar Sasselov | Zendy

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Dispersing the Gaseous Protoplanetary Disk and Halting Type II Migration

Author(s) -

M. Lecar,

Dimitar Sasselov

Publication year - 2003

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/379207

Subject(s) - planet , physics , exoplanet , protoplanetary disk , planetary migration , photoevaporation , astrophysics , planetary mass , debris disk , astronomy , outer planets , thick disk , planetary system , terrestrial planet , halo , galaxy

More than 30 extra-solar Jupiter-like planets have shorter periods than theplanet Mercury. It is generally accepted that they formed further out, andmigrated inwards. In order to be driven by tidal torques from the gaseous disc,the disc exterior to the planet had to contain about a planetary mass. The factthat the planets stopped migrating means that their outer disc was removed. Wesuggest that the outer disc was accreted by the planet. In this scenario, theendgame is a race. The planet survives if it accretes its outer disc beforebeing accreted by the star. The winner is determined solely by the ratio of themass of the outer disc to the local surface density of the disc.Comment: 5 pages, submitted to ApJ

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