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An Accretion Model for the Growth of Black Hole in QuasarsA possible accretion model associated with the ionization instability of quasar disks is proposed to address the growth of the central black hole harbored in the host galaxy. The evolution of quasars in cosmic time is assumed to change from a highly active state to a quiescent state triggered by the S-shaped ionization instability of the quasar accretion disk. For a given external mass transfer rate ionization instability can modify accretion rate in the disk and separates the accretion flows of the disk into three different phases like a S-shape. We suggest that the bright quasars observed today are those quasars with disks in the upper branch of S-shaped instability and the dormant quasars are the system in the lower branch. The disk is assumed to evolve as ADIOS configuration in the lower branch. The mass ratio between black hole and its host galactic bulge is a nature consequence of ADIOS. Our model also demonstrates that a seed black hole 2 x 10(exp 6) solar masses similar to those found in spiral galaxies today is needed to produce a black hole with a final mass 2 x 10(exp 8) solar masses.
Document ID
20040071162
Acquisition Source
Headquarters
Document Type
Conference Paper
Authors
Lu, Ye
(Beijing Univ. China)
Cheng, K. S.
(Yunnan Univ. Kunming, China)
Zhang, S. N.
(Alabama Univ. Huntsville, AL, United States)
Date Acquired
August 21, 2013
Publication Date
July 1, 2003
Subject Category
Astrophysics
Meeting Information
Meeting: Quasar Cores and Jets: 25th Meeting of the IAU
Location: Sydney
Country: Australia
Start Date: July 23, 2003
End Date: July 24, 2003
Sponsors: International Astronomical Union
Funding Number(s)
CONTRACT_GRANT: NAG5-7927
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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