A self-consistent solution for an accretion disc structure around a rapidly rotating non-magnetized star

Details A self-consistent solution for an accretion disc structure around a rapidly rotating non-magnetized star A self-consistent solution for an accretion disc structure around a rapidly rotating non-magnetized star

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...274..796b&link_type=abstract

Astronomy and Astrophysics, Vol. 274, p. 796 (1993)

Astronomy and Astrophysics

Astrophysics

16

Accretion Disks, Hydrodynamics, Stars: Neutron, X-Rays: Stars

Scientific paper

When an accretion disc increase the stellar angular velocity to a critical value, a self-consistent regime of accretion is established, in which the specific angular momentum of the acereting matter is equal to the mass derivative of the angular momentum of the star along the sequence of the critically rotating states. Self-consistent regimes are investigated for rigidly rotating stars, where viscosity is large, as well as in the case of existence of a self-similar solution, in which the stellar structure and angular velocity law do not depend on stellar mass for an appropriate choice of non-dimensional variables. The rotation law does not deviate strongly from rigid rotation in any case, so it is always possible to use the parameters of rigidly rotating stars in order to obtain an approximation of the structure of the accretion disc. For known stellar parameters, simple recipes are given for obtaining the structure and luminosity of the accretion disc from the known accretion disc structure around a black hole. Luminosity variations of accretion disc are estimated when the acereting star approaches critical rotation. These variations could happen in LMXB, cataclysmic variables and rapidly rotating pre-main-sequence stars of T Tauri type with accretion discs.

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