MG11 
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Abstract

Gravitational wave damping from a self-gravitating vibrating ring of matter around a black hole

We consider the space time structure of a black hole - ring system in which a non-rotating black hole is surrounded by a gravitating disk, here simplified to be a ring. We use Weyl co-ordinate to solve for the metric and compute the behaviour of the time-like geodesics. We then consider the purturbation of the ring and see how the purturbation dampens after emission of the gravitational waves

Gravitational wave emission from a stellar companion black hole in presence of an accretion disk around a Kerr black hole

We consider a system consisting of a binary black hole system, one massive and rotating, while the other is a stellar mass which is moving through an accretion disk which surrounds the massive black hole. We find the angular momentum distrubution self-consistently inside the disk and determine the exchange of angular momentum between the companion black hole and the accretion disk. We find that the gravitational wave profile will be vastly different depending on the flow parameter of the accretion disk. We show these profiles When these disks have accretion shocks, the profile also suddenly changes. In combination with electromagnetic spectral information this gravitational wave information would allow us to extract parameters such as the spin of the central black hole, mass accretion rates, mass of the black holes etc.

Gravitational wave emission from a stellar companion black hole in presence of an accretion disk around a Kerr black hole

We consider a system consisting of a binary black hole system, one massive and rotating, while the other is a stellar mass which is moving through an accretion disk which surrounds the massive black hole. We find the angular momentum distrubution self-consistently inside the disk and determine the exchange of angular momentum between the companion black hole and the accretion disk. We find that the gravitational wave profile will be vastly different depending on the flow parameter of the accretion disk. We show these profiles When these disks have accretion shocks, the profile also suddenly changes. In combination with electromagnetic spectral information this gravitational wave information would allow us to extract parameters such as the spin of the central black hole, mass accretion rates, mass of the black holes etc.

Gravitational wave emission from a stellar companion black hole in presence of an accretion disk around a Kerr black hole

We consider a system consisting of a binary black hole system, one massive and rotating, while the other is a stellar mass which is moving through an accretion disk which surrounds the massive black hole. We find the angular momentum distrubution self-consistently inside the disk and determine the exchange of angular momentum between the companion black hole and the accretion disk. We find that the gravitational wave profile will be vastly different depending on the flow parameter of the accretion disk. We show these profiles When these disks have accretion shocks, the profile also suddenly changes. In combination with electromagnetic spectral information this gravitational wave information would allow us to extract parameters such as the spin of the central black hole, mass accretion rates, mass of the black holes etc.

Solution topologies of a viscous advective accretion flows around a Kerr black hole

In the literature, viscous advective flows have been studied around a non-rotating black hole. It had been observed that depending on the viscosity parameter the flow may or may not have more than one saddle type sonic points. Here we generalize the work using pseudo-Kerr geometry and found the sonic points and the location of the shock waves as functions of the Kerr parameter. We also include the effects of the viscous heating and bremsstrahlung cooling processes occuring in the accretion flow.