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Article: High energy radiation from the direction of the galactic black hole Sgr A*

TitleHigh energy radiation from the direction of the galactic black hole Sgr A*
Authors
Keywordsγ-rays
Galactic black hole
Radiation processes
Issue Date2008
PublisherPergamon. The Journal's web site is located at http://www.elsevier.com/locate/asr
Citation
Advances In Space Research, 2008, v. 42 n. 3, p. 538-543 How to Cite?
AbstractX-ray observations indicate that the Galactic black hole Sgr A* is inactive now, however, we suggest that Sgr A* can become active when a captured star is tidally disrupted and matter is accreted into the black hole. Consequently the Galactic black hole could be a powerful source of relativistic protons with a characteristic energy ∼1052 erg per capture. The diffuse GeV and TeV γ-rays emitted in the direction of the Galactic Center (GC) are the direct consequences of p-p collisions of such relativistic protons ejected by very recent capture events occurred ≤105 yr ago. On the other hand, the extended electron-positron annihilation line emission observed from GC is a phenomenon related to a large population of thermalized positrons, which are produced, cooled down and accumulated through hundreds of past capture events during a period of ∼107 yr. In addition to explaining GeV, TeV and 511 keV annihilation emissions we also estimate the photon flux of several MeV resulting from in-flight annihilation process. © 2007 COSPAR.
Persistent Identifierhttp://hdl.handle.net/10722/80450
ISSN
2015 Impact Factor: 1.409
2015 SCImago Journal Rankings: 0.606
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorChernyshov, DOen_HK
dc.contributor.authorDogiel, Ven_HK
dc.date.accessioned2010-09-06T08:06:35Z-
dc.date.available2010-09-06T08:06:35Z-
dc.date.issued2008en_HK
dc.identifier.citationAdvances In Space Research, 2008, v. 42 n. 3, p. 538-543en_HK
dc.identifier.issn0273-1177en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80450-
dc.description.abstractX-ray observations indicate that the Galactic black hole Sgr A* is inactive now, however, we suggest that Sgr A* can become active when a captured star is tidally disrupted and matter is accreted into the black hole. Consequently the Galactic black hole could be a powerful source of relativistic protons with a characteristic energy ∼1052 erg per capture. The diffuse GeV and TeV γ-rays emitted in the direction of the Galactic Center (GC) are the direct consequences of p-p collisions of such relativistic protons ejected by very recent capture events occurred ≤105 yr ago. On the other hand, the extended electron-positron annihilation line emission observed from GC is a phenomenon related to a large population of thermalized positrons, which are produced, cooled down and accumulated through hundreds of past capture events during a period of ∼107 yr. In addition to explaining GeV, TeV and 511 keV annihilation emissions we also estimate the photon flux of several MeV resulting from in-flight annihilation process. © 2007 COSPAR.en_HK
dc.languageengen_HK
dc.publisherPergamon. The Journal's web site is located at http://www.elsevier.com/locate/asren_HK
dc.relation.ispartofAdvances in Space Researchen_HK
dc.subjectγ-raysen_HK
dc.subjectGalactic black holeen_HK
dc.subjectRadiation processesen_HK
dc.titleHigh energy radiation from the direction of the galactic black hole Sgr A*en_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0273-1177&volume=42&spage=538&epage=543&date=2008&atitle=High+energy+radiation+from+the+direction+of+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.asr.2007.04.103en_HK
dc.identifier.scopuseid_2-s2.0-44849118538en_HK
dc.identifier.hkuros143381en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-44849118538&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume42en_HK
dc.identifier.issue3en_HK
dc.identifier.spage538en_HK
dc.identifier.epage543en_HK
dc.identifier.isiWOS:000257684300021-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridChernyshov, DO=14059433800en_HK
dc.identifier.scopusauthoridDogiel, V=6603566238en_HK

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