The stability of spherically symmetric accretion flows

Details The stability of spherically symmetric accretion flows The stability of spherically symmetric accretion flows

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979ap%26ss..66..277a&link_type=abstract

Astrophysics and Space Science, vol. 66, no. 2, Dec. 1979, p. 277-285.

Computer Science

Numerical Analysis

1

Flow Stability, Magnetohydrodynamic Flow, Numerical Analysis, Stellar Mass Accretion, X Ray Astronomy, Critical Flow, Eigenvalues, Eigenvectors, Euler-Lagrange Equation, Flow Velocity, High Temperature Plasmas, Isothermal Flow, Subsonic Flow

Scientific paper

An examination of spherically symmetric accretion flows is presented, including an analytical proof on stability for isothermal critical flow by a method similar to Jocker's (1968) stability theory, and numerical stability analyses for critical accretion flows. The treatment involves fundamental equations for stationary accretion flows and for spherically symmetric perturbations (SSPs), and boundary conditions. It is concluded that critical accretion flows for any values of gamma in the range greater than or equal to 1 and less than 5/3 are stable with respect to the normal and drift modes of SSPs, and that the subsonic and Type I critical flows are unstable with respect to the normal mode; this agrees with Bondi's (1952) idea that accretion takes place at the greatest possible rate.

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