Planet migration: self-gravitating radiation hydrodynamical models of protoplanets with surfaces - Astrophysics > Earth and Planetary AstrophysicsReportar como inadecuado




Planet migration: self-gravitating radiation hydrodynamical models of protoplanets with surfaces - Astrophysics > Earth and Planetary Astrophysics - Descarga este documento en PDF. Documentación en PDF para descargar gratis. Disponible también para leer online.

Abstract: We calculate radial migration rates of protoplanets in laminar minimum masssolar nebula discs using three-dimensional self-gravitating radiationhydrodynamical RHD models. The protoplanets are free to migrate, whereupontheir migration rates are measured. For low mass protoplanets 10-50 M \opluswe find increases in the migration timescales of up to an order of magnitudebetween locally-isothermal and RHD models. In the high-mass regime themigration rates are changed very little. These results are arrived at bycalculating migration rates in locally-isothermal models, before sequentiallyintroducing self-gravity, and radiative transfer, allowing us to isolate theeffects of the additional physics. We find that using a locally-isothermalequation of state, without self-gravity, we reproduce the migration ratesobtained by previous analytic and numerical models. We explore the impact ofdifferent protoplanet models, and changes to their assumed radii, uponmigration. The introduction of self-gravity gives a slight reduction of themigration rates, whilst the inertial mass problem, which has been proposed forhigh mass protoplanets with circumplanetary discs, is reproduced. Uponintroducing radiative transfer to models of low mass protoplanets \approx 10M \oplus, modelled as small radius accreting point masses, we find outwardmigration with a rate of approximately twice the analytic inward rate. However,when modelling such a protoplanet in a more realistic manner, with a surfacewhich enables the formation of a deep envelope, this outward migration is notseen.



Autor: Ben A. Ayliffe, Matthew R. Bate

Fuente: https://arxiv.org/







Documentos relacionados