QPOs expected in rotating accretion flows around a supermassive black hole

Details QPOs expected in rotating accretion flows around a supermassive black hole QPOs expected in rotating accretion flows around a supermassive black hole

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..423o&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Computer Science

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Scientific paper

It is well known that rotating inviscid accretion flows with adequate injection parameters around black holes could form shock waves close to the black holes, after the flow passes through the outer sonic point and can be virtually stopped by the centrifugal force. We numerically examine such shock waves in low-angular momentum 2D accretion flows around a supermassive black hole with 106 solar mass, while taking account of the cooling and heating of the gas and the radiation transport. For a set of the injection parameters, such as the specific angular momentum, the radial velocity, and the sound velocity at an outer boundary, the accretion flows with 10(-3) to 106 Eddington critical accretion rates form shock waves close to the black hole. The shocks locate at 6 - 12 Schwartzschild radii, depending on the accretion rate, and oscillate quasi-periodically around the shock position. The resultant luminosities show QPOs with modulations of a factor 3 and with quasi-periods of a few to several hours. This suggests the existence of QPOs with the time-scale of hours in AGNs. The luminosities of the accretion flows increase in proportion to the accretion rate when it is low, but they tend to a saturated value of 3.3 Eddington luminosity when it exceeds considerably the Eddington critical rate. In these luminous accretion flows, the relativistic mass-outflow is also found in the very hot and rarefied region along the rotational axis, where the mass-outflow rate is as high as a few percent of the input accretion rate.

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