6533b7cffe1ef96bd1259087
RESEARCH PRODUCT
Steady state shocks in accretion disks around a Kerr black hole
Diego MolteniH. Sponholzsubject
PhysicsSupermassive black holeActive galactic nucleusAstrophysics::High Energy Astrophysical PhenomenaAstrophysics (astro-ph)FOS: Physical sciencesAstronomy and AstrophysicsQuasarAstrophysicsGeneral Relativity and Quantum Cosmology (gr-qc)Astrophysics::Cosmology and Extragalactic AstrophysicsAstrophysicsGeneral Relativity and Quantum CosmologyGeneral Relativity and Quantum CosmologyBinary black holeRotating black holeSpace and Planetary ScienceIntermediate-mass black holeStellar black holeSpin-flipAstrophysics::Earth and Planetary AstrophysicsAstrophysics::Galaxy Astrophysicsdescription
Results of numerical simulations of shock solutions in a geometrical thin accretion disk around a Kerr black hole (BH) are presented. Using the smoothed particle hydrodynamics (SPH) technique, the influence of the central object is included by means of an effective potential, We first present the theory of standing shock formation in accretion disks around a Kerr black hole, and show that the results of our numerical simulation agree very well with the theoretical results. We find that the shocks in an inviscid flow are very stable. We also remove the ambiguity prevalent regarding the location and stability of shocks in adiabatic flows. Finally we sketch some of the astrophysical consequences of our findings in relation to accretion disks in Active Galactic Nuclei (AGN) and Quasars.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 1994-11-01 |