Black Hole Disk Accretion in Supernovae

Details Black Hole Disk Accretion in Supernovae Black Hole Disk Accretion in Supernovae

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...489..227m&link_type=abstract

Astrophysical Journal v.489, p.227

Physics

26

Accretion, Accretion Disks, Black Hole Physics, Stars: Supernovae: General

Scientific paper

Massive stars in a certain mass range may form low-mass black holes after supernova explosions. In such massive stars, fallback of ~0.1 M&sun; materials onto a black hole is expected because of a deep gravitational potential or a reverse shock propagating back from the outer composition interface. We study hydrodynamical disk accretion onto a newborn low-mass black hole in a supernova using the smoothed particle hydrodynamics method. If the progenitor was rotating before the explosion, the fallback material should have a certain amount of angular momentum with respect to the black hole, thus forming an accretion disk. The disk material will eventually accrete toward the central object because of viscosity at a supercritical accretion rate, M dot /M dot _{{crit}}>106 , for the first several tens of days. (Here, M dot _{{crit}} is the Eddington luminosity divided by c2.) We then expect that such an accretion disk is optically thick and advection dominated; that is, the disk is so hot that the produced energy and photons are advected inward rather than being radiated away. Thus, the disk luminosity is much less than the Eddington luminosity. The disk becomes hot and dense; for M dot /M dot _{{crit}}~106 , for example, T ~ 109( alpha vis/0.01)-1/4 K and rho ~ 103( alpha vis/0.01)-1 g cm-3 (with alpha vis being the viscosity parameter) in the vicinity of the black hole. Depending on the material mixing, some interesting nucleosynthesis processes via rapid proton and alpha-particle captures are expected even for reasonable viscosity magnitudes ( alpha vis ~ 0.01), and some of them could be ejected in a disk wind or a jet without being swallowed by the black hole.

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