riassunto2

Speaker	Saijo, Motoyuki
Co-autors	*Ian Hawke*
Talk Title	Collapse of a differentially rotating supermassive star to a supermassive black hole
Abstract	We investigate the collapse of differentially rotating supermassive stars (SMSs) by means of 3+1 hydrodynamic simulations in general relativity. We find that the estimated ratio between the black hole (BH) and the surrounding disk from the equilibrium star is roughly the same as the results from numerical simulation. We also find that there exists a quasi-periodic waves after the quasinormal mode frequency dumped out where the disk has formed. Furthermore, when the newly formed BH is almost an extreme Kerr, the amplitude of a quasi-periodic oscillation enhances throughout the evolution. Geometrical feature, shock waves, instabilities of the fluid are suggested as a cause of this amplification behaviour. This alternative scenario for the collapse of differentially rotating SMSs might be observable by LISA.
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