Bondi Accretion onto a Luminous Object

Details Bondi Accretion onto a Luminous Object Bondi Accretion onto a Luminous Object

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001pasj...53..687f&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.53, No. 4, pp. 687-692

Physics

3

Accretion, Accretion Disk, Black Hole Physics, Radiation Mechanism: General, X-Rays: Stars

Scientific paper

Spherical accretion of ionized gas onto a gravitating object is examined under the influence of central radiation. In classical Bondi accretion onto a non-luminous source with mass M, the accretion rate dot{M}B is expressed as dot{M}B = λ(γ) × 4πG2M2ρinfty c-3s infty, where ρinfty is the density at infinity and cs infty the sound speed at infinity. We first found that the normalized accretion rate λ(γ) is approximated by λ(γ) = -(5/4)γ + (19/8), instead of a rigorous expression. When the central object is a ``spherical'' source, the accretion rate dot{M} reduces to dot{M}B(1-Γ)2, where Γ is the central luminosity normalized by the Eddington one. If the central luminosity is produced by the accretion energy, the steady canonical luminosity is determined and the normalized luminosity does not exceed unity, as expected. On the other hand, when the central object is a ``disk'' source, such as an accretion disk, the accretion rate becomes dot{M}/dot{M}B = 1 - 2Γd + (4/3)Γ2d for Γd leq 1/2, and dot{M}/dot{M}B = 1/(6Γd for Γd < 1/2, where Γd is the normalized disk luminosity. We also found steady canonical solutions, where the normalized luminosity can exceed unity for sufficiently large accretion rates. The anisotropic radiation field of accretion disks greatly modifies the accretion nature.

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