A two-zone model of the boundary layer of an accretion disk

Details A two-zone model of the boundary layer of an accretion disk A two-zone model of the boundary layer of an accretion disk

Mar 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000newa....5...43a&link_type=abstract

New Astronomy, vol. 5, no. 1, p. 43-52.

Astronomy and Astrophysics

Astronomy

Scientific paper

A two-zone model of the optically thick transition zone between a Keplerian, i.e., geometrically thin accretion disk and a slowly rotating accreting star is introduced. In contrast to an infinitely thin standard model boundary layer or a one-zone model, this boundary layer is permitted to "cool" by dumping energy into the Keplerian disk. The Keplerian disk is heated significantly in the new model, which leads to a "heated Keplerian layer". This situation is modeled in the present paper, leading to results that agree with complex numerical calculations.

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