Numerical Simulations of Rotating Accretion Flows near a Black Hole

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dc.creatorRyu, Dongsu
dc.creatorChakrabarti, Sandip K.
dc.date1997-02-05
dc.date.accessioned2026-07-07T02:22:53Z
dc.date.available2026-07-07T02:22:53Z
dc.descriptionWe present time-dependent solutions of thin, supersonic accretion flows near a black hole and compare them with analytical solutions. Such flows of inviscid, adiabatic gas are characterized by the specific angular momentum and the specific energy. We confirm that for a wide range of above parameters a stable standing shock wave with a vortex inside it forms close to the black hole. Apart from steady state solutions, we show the existence of non-steady solutions for thin accretion flows where the accretion shock is destroyed and re-generated periodically. The unstable behavior should be caused by dynamically induced instabilities, since inviscid, adiabatic gas is considered. We discuss possible relevance of the periodic behavior on quasi-periodic oscillations (QPOs) observed in galactic and extragalactic black hole candidates.
dc.description6 pages with 3 figures, uses paspconf.sty, to appear in "Computational Astrophysics", the Proceedings of the 12th Kingston Meeting ed. D. Clarke & M. West, also available upon request to ryu@hermes.astro.washington.edu
dc.identifierhttps://arxiv.org/abs/astro-ph/9702054
dc.identifierhttp://arxiv.org/abs/astro-ph/9702054
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/11045
dc.subjectAstrophysics
dc.titleNumerical Simulations of Rotating Accretion Flows near a Black Hole
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