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Article: An accretion model for the growth of the central black hole associated with ionization instability in quasars

TitleAn accretion model for the growth of the central black hole associated with ionization instability in quasars
Authors
KeywordsAccretion, accretion disks
Black hole physics
Galaxies: active
Galaxies: bulges
Galaxies: nuclei
Quasars: general
Issue Date2003
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2003, v. 590 n. 1 I, p. 52-57 How to Cite?
AbstractA possible accretion model associated with the ionization instability of quasar disks is proposed to address the growth of the central black hole (BH) 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 Mext supplied by the quasar host galaxy, ionization instability can modify the accretion rate in the disk and separate the accretion flows of the disk into three different phases, like an S-shape. We suggest that the bright quasars observed today are those quasars with disks in the upper branch of the S-shaped instability, and the faint or "dormant" quasars are simply these systems in the lower branch. The middle branch is the transition state, which is unstable. We assume the quasar disk evolves according to the advection-dominated inflow-outflow solution (ADIOS) configuration in the stable lower branch of the S-shaped instability, and the Eddington accretion rate is used to constrain the accretion rate in the highly active phase. The mass ratio between a BH and its host galactic bulge is a natural consequence of an ADIOS. Our model also demonstrates that a seed BH (∼2 × 106 M⊙) similar to those found in spiral galaxies today is needed to produce a BH with a final mass of ∼2 × 108 M⊙.
Persistent Identifierhttp://hdl.handle.net/10722/43388
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLu, Yen_HK
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorZhang, SNen_HK
dc.date.accessioned2007-03-23T04:44:45Z-
dc.date.available2007-03-23T04:44:45Z-
dc.date.issued2003en_HK
dc.identifier.citationAstrophysical Journal Letters, 2003, v. 590 n. 1 I, p. 52-57en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43388-
dc.description.abstractA possible accretion model associated with the ionization instability of quasar disks is proposed to address the growth of the central black hole (BH) 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 Mext supplied by the quasar host galaxy, ionization instability can modify the accretion rate in the disk and separate the accretion flows of the disk into three different phases, like an S-shape. We suggest that the bright quasars observed today are those quasars with disks in the upper branch of the S-shaped instability, and the faint or "dormant" quasars are simply these systems in the lower branch. The middle branch is the transition state, which is unstable. We assume the quasar disk evolves according to the advection-dominated inflow-outflow solution (ADIOS) configuration in the stable lower branch of the S-shaped instability, and the Eddington accretion rate is used to constrain the accretion rate in the highly active phase. The mass ratio between a BH and its host galactic bulge is a natural consequence of an ADIOS. Our model also demonstrates that a seed BH (∼2 × 106 M⊙) similar to those found in spiral galaxies today is needed to produce a BH with a final mass of ∼2 × 108 M⊙.en_HK
dc.format.extent120876 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectAccretion, accretion disksen_HK
dc.subjectBlack hole physicsen_HK
dc.subjectGalaxies: activeen_HK
dc.subjectGalaxies: bulgesen_HK
dc.subjectGalaxies: nucleien_HK
dc.subjectQuasars: generalen_HK
dc.titleAn accretion model for the growth of the central black hole associated with ionization instability in quasarsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=590&issue=1 pt 1&spage=52&epage=57&date=2003&atitle=An+Accretion+Model+for+the+Growth+of+the+Central+Black+Hole+Associated+with+Ionization+Instability+in+Quasarsen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/375007en_HK
dc.identifier.scopuseid_2-s2.0-0042655470en_HK
dc.identifier.hkuros77191-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0042655470&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume590en_HK
dc.identifier.issue1 Ien_HK
dc.identifier.spage52en_HK
dc.identifier.epage57en_HK
dc.identifier.isiWOS:000183278700006-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridLu, Y=7405476987en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridZhang, SN=14061519700en_HK

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