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Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

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In this talk, I will present results of our recent 3D GRHD simulations of thick accretion disks around tilted Kerr black holes.  We investigate the effects of the tilt angle between the disk angular momentum vector and black hole spin on the dynamics of these systems, being particularly interested in a possible imprint of the tilt angle in the gravitational wave pattern as the torus evolves in the tilted spacetime. We find that Papalouizou-Pringle unstable models still develop the PPI when the central BH is tilted. For the models where the PPI saturates abruptly, the central BH is given a mild kick. We simulate the systems using the Einstein Toolkit, using the thorn McLachlan for the evolution of the spacetime via the BSSN formalism and the thorn GRHydro for the evolution of the hydrodynamics, using a 3D Cartesian mesh with adaptive mesh refinement (AMR).

Seminar of F. Vincent (PAS, Warsaw)

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Frederic Vincent from the Polish Academy of Sciences will give a talk on Tuesday, February 11, at 12:00.

The talk will be held at the ITP, Room 2.114, Max-von-Laue-Str. 1.

Title: Black hole variability: from Galactic Center flares to microquasars oscillations

Abstract:
Black hole systems can be affected by variable phenomena. This temporal variability scales with the mass of the black hole and it is thus likely that it is related with strong-field gravity. This seminar is dedicated to examining some possible scenarios of black hole variability and linking them when possible to future observations. During this talk, he will discuss two kind of variable phenomena:
1) the Galactic Center flares of radiation, presenting simulations of astrometric observations of flares by the very-near future (May 2015) infrared interferometer GRAVITY and discussing the possibility that GRAVITY could help distinguish different theoretical flare scenarios;
2) microquasars oscillations, presenting a model of microquasar high-frequency quasiperiodic oscillations, namely the oscillating torus model, a simulated temporal power spectra for this model and discussing them in the perspective of the 3:2 resonance that some microquasars exhibit.