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Article: High Energy Radiation from the Galactic Black Hole Sgr A*

TitleHigh Energy Radiation from the Galactic Black Hole Sgr A*
Authors
Issue Date2008
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/npbps
Citation
Nuclear Physics B - Proceedings Supplements, 2008, v. 175-176 SUPPL.: COMPLETE, p. 383-388 How to Cite?
AbstractWe suggest that the energy source of the observed TeV, GeV and 511 KeV annihilation lines from the direction of the Galactic Center is the Galactic black hole Sgr A*, which becomes active when a captured star is tidally disrupted and matter is accreted into the black hole. During the active phase relativistic protons are ejected. GeV-TeV photons result from the decay of neutral pions produced by proton-proton collisions. Positrons lost most of their energies in the central region and diffuse to 500 pc region, where they cool to several eV via ionization loss. 511 KeV lines are produced by these thermalized positrons through the decay of positronium in warm gas. It is extremely important to notice that the energy injection is not continuous because the capture event only takes place once every 105yr and the gas density in the Galactic Center is non-uniform. We compare the observed data with model predictions. © 2007 Elsevier B.V. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/80443
ISSN
2005 Impact Factor: 0.875
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorChernyshov, DOen_HK
dc.contributor.authorDogiel, Ven_HK
dc.date.accessioned2010-09-06T08:06:30Z-
dc.date.available2010-09-06T08:06:30Z-
dc.date.issued2008en_HK
dc.identifier.citationNuclear Physics B - Proceedings Supplements, 2008, v. 175-176 SUPPL.: COMPLETE, p. 383-388en_HK
dc.identifier.issn0920-5632en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80443-
dc.description.abstractWe suggest that the energy source of the observed TeV, GeV and 511 KeV annihilation lines from the direction of the Galactic Center is the Galactic black hole Sgr A*, which becomes active when a captured star is tidally disrupted and matter is accreted into the black hole. During the active phase relativistic protons are ejected. GeV-TeV photons result from the decay of neutral pions produced by proton-proton collisions. Positrons lost most of their energies in the central region and diffuse to 500 pc region, where they cool to several eV via ionization loss. 511 KeV lines are produced by these thermalized positrons through the decay of positronium in warm gas. It is extremely important to notice that the energy injection is not continuous because the capture event only takes place once every 105yr and the gas density in the Galactic Center is non-uniform. We compare the observed data with model predictions. © 2007 Elsevier B.V. All rights reserved.en_HK
dc.languageengen_HK
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/npbpsen_HK
dc.relation.ispartofNuclear Physics B - Proceedings Supplementsen_HK
dc.rightsNuclear Physics, Section B, Proceedings Supplements. Copyright © Elsevier BV.en_HK
dc.titleHigh Energy Radiation from the Galactic Black Hole Sgr A*en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0920-5632&volume=175-176&spage=383&epage=388&date=2008&atitle=High+energy+radiation+from+the+Galactic+black+hole+Sgr+A*en_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1016/j.nuclphysbps.2007.11.036en_HK
dc.identifier.scopuseid_2-s2.0-37649007105en_HK
dc.identifier.hkuros139862en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-37649007105&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume175-176en_HK
dc.identifier.issueSUPPL.: COMPLETEen_HK
dc.identifier.spage383en_HK
dc.identifier.epage388en_HK
dc.publisher.placeNetherlandsen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridChernyshov, DO=14059433800en_HK
dc.identifier.scopusauthoridDogiel, V=6603566238en_HK

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