Statistics – Computation
Scientific paper
Oct 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...184..173s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 184, no. 1-2, Oct. 1987, p. 173-184.
Statistics
Computation
122
Accretion Disks, Magnetohydrodynamics, Shock Waves, Computational Astrophysics, Roche Limit
Scientific paper
Special solutions of the equations of motion and continuity near the midplane of a thin accretion disk are obtained by analytic and numerical means. They have the form of stationary, self-similar flows containing two or more spiral shaped shock waves. They represent shocks initiated by a disturbance at the outer edge of the disk. Self-similar shocks excited at the center of the disk do not seem to exist. No solutions were found containing only one shock. Adiabatically accreting solutions exist in which there is a unique relation between the ratio of specific heats γ and the opening angle of the shock. When radiative losses from the disk are included, solutions exist for γ above a certain minimum value. The strength of the shock decreases with decreasing disk thickness. An effective "α parameter" can be defined, it varies with disk thickness like (h/r)1.5. An analogy between the present problem and the case of spherically symmetric accretion is discussed.
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