Steady-state shocks in an accretion disc around a Kerr black hole | Zendy

H. Sponholz | Zendy; D. Molteni | Zendy

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Steady-state shocks in an accretion disc around a Kerr black hole

Author(s) -

H. Sponholz,

D. Molteni

Publication year - 1994

Publication title -

monthly notices of the royal astronomical society

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.058

H-Index - 383

eISSN - 1365-8711

pISSN - 0035-8711

DOI - 10.1093/mnras/271.1.233

Subject(s) - physics , accretion (finance) , rotating black hole , active galactic nucleus , astrophysics , black hole (networking) , kerr metric , adiabatic process , shock wave , inviscid flow , quasar , smoothed particle hydrodynamics , classical mechanics , schwarzschild radius , mechanics , galaxy , computer network , routing protocol , routing (electronic design automation) , computer science , thermodynamics , link state routing protocol

Results of numerical simulations of shock solutions in a geometrical thinaccretion disk around a Kerr black hole (BH) are presented. Using the smoothedparticle hydrodynamics (SPH) technique, the influence of the central object isincluded by means of an effective potential, We first present the theory ofstanding shock formation in accretion disks around a Kerr black hole, and showthat the results of our numerical simulation agree very well with thetheoretical results. We find that the shocks in an inviscid flow are verystable. We also remove the ambiguity prevalent regarding the location andstability of shocks in adiabatic flows. Finally we sketch some of theastrophysical consequences of our findings in relation to accretion disks inActive Galactic Nuclei (AGN) and Quasars.Comment: 9 pages (figures included) self-extracting compressed PostScript, in press (MNRAS

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