The structure of protosolar accretion disk

Details The structure of protosolar accretion disk The structure of protosolar accretion disk

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001acasn..42....1l&link_type=abstract

Acta Astronomical Sinica, vol.42, no.1, p. 1-8.

Astronomy and Astrophysics

Astronomy

2

Protosun, Accretion Disk, Convection, Radiation

Scientific paper

The structure of protosolar accretion disk during viscous diffusion stage is calculated. The standard αmodel is used to describe the viscosity in the optically thick protosolar accretion disc. The energy transport associated with radial motions is neglected and the vertical structure is constructed by assuming a Keplerian rotation and local hydrostatic and thermal equilibrium. The disk is heated by viscous dissipation and energy is transported by convection or radiation. It is found that the dependence of opacity on temperature is important to the disk structure. For the cold protosolar accretion disc, convective instability will gradually end from the outer region to the center and from the surface to central plane. So the formation of planets should first take place in the region where convection ends.

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