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Article: Nuclear interaction gamma-ray lines from the Galactic center region

TitleNuclear interaction gamma-ray lines from the Galactic center region
Authors
KeywordsGalaxy: center
Gamma rays: theory
Radiation mechanisms: non-thermal
Issue Date2009
PublisherE D P Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2009, v. 508 n. 1, p. 1-7 How to Cite?
AbstractAims. The accretion of stars onto the central supermassive black hole at the center of the Milky Way is predicted to generate large fluxes of subrelativistic ions in the Galactic center region. We analyze the intensity, shape, and spatial distribution of de-excitation gamma-ray lines produced by nuclear interactions of these energetic particles with the ambient medium. Methods. We first estimated the amount and mean kinetic energy of particles released from the central black hole during star disruption. We then calculated the energy and spatial distributions of these particles in the Galactic center region from a kinetic equation. These particle distributions were then used to derive the characteristics of the main nuclear interaction gamma-ray lines.Results. Because the time period of star capture by the supermassive black hole is expected to be shorter than the lifetime of the ejected fast particles against Coulomb losses, the gamma-ray emission is predicted to be stationary. We find that the nuclear de-excitation lines should be emitted from a region with a maximum 5° angular radius. The total gamma-ray line flux below 8 MeV is calculated to be ̃ 10 -4 photons cm -2 s -1. The most promising lines for detection are those at 4.44 and ~6.2 MeV, with a predicted flux in each line of ̃10 -5 photons cm -2 s -1. Unfortunately, it is unlikely that this emission can be detected with the INTEGRAL observatory. But the predicted line intensities appear to be within reach of future gamma-ray space instruments. A future detection of de-excitation gamma-ray lines from the Galactic center region would provide unique information on the high-energy processes induced by the central supermassive black hole and the physical conditions of the emitting region. © 2009 ESO.
Persistent Identifierhttp://hdl.handle.net/10722/80496
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
ISI Accession Number ID
Funding AgencyGrant Number
RFBR08-02-00170-a
NSC-RFBR Joint Research ProjectRP09N04
09-02-92000-HHC-a
President of the Russian Federation
Hong Kong GovernmentHKU 7014/07P
National Basic Research Program of China2009CB824800
Taiwan National Science CouncilNSC 96-2112-M-008-014-MY3
NSC-982923- M-008-001-MY3
NSC 96-2752-M-008-011-PAE
NSC 96-2111-M-008-010
Funding Information:

First of all we would like to mention that the referee's report was very helpful for us and we thank him for comments. The authors are also grateful to H.-K. Chang, Y. Chou, Ya. N. Istomin, and Y. Maeda, for helpful discussions, and to W. Hermsen and H. Bloemen for valuable input. V. A. D. and D. O. C. are partly supported by the RFBR grant 08-02-00170-a, the NSC-RFBR Joint Research Project RP09N04 and 09-02-92000-HHC-a, and by the grant of the President of the Russian Federation "Scientific School of Academician V. L. Ginzburg". K. S. C. is supported by an RGC grant of the Hong Kong Government under HKU 7014/07P and a National Basic Research Program of China under 2009CB824800. C. M. K. is supported by the Taiwan National Science Council grants NSC 96-2112-M-008-014-MY3 and NSC-982923- M-008-001-MY3. W. H. I. is supported by the Taiwan National Science Council grants NSC 96-2752-M-008-011-PAE and NSC 96-2111-M-008-010. The last version of the paper was partly prepared in ISAS/JAXA (Sagamihara, Japan). V. A. D. thanks ISAS and particularly Prof. Kazuhisa Mitsuda and the ISAS director Prof. Hajime Inoue for hospitality.

References

 

DC FieldValueLanguage
dc.contributor.authorDogiel, VAen_HK
dc.contributor.authorTatischeff, Ven_HK
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorChernyshov, DOen_HK
dc.contributor.authorKo, CMen_HK
dc.contributor.authorIp, WHen_HK
dc.date.accessioned2010-09-06T08:07:05Z-
dc.date.available2010-09-06T08:07:05Z-
dc.date.issued2009en_HK
dc.identifier.citationAstronomy And Astrophysics, 2009, v. 508 n. 1, p. 1-7en_HK
dc.identifier.issn0004-6361en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80496-
dc.description.abstractAims. The accretion of stars onto the central supermassive black hole at the center of the Milky Way is predicted to generate large fluxes of subrelativistic ions in the Galactic center region. We analyze the intensity, shape, and spatial distribution of de-excitation gamma-ray lines produced by nuclear interactions of these energetic particles with the ambient medium. Methods. We first estimated the amount and mean kinetic energy of particles released from the central black hole during star disruption. We then calculated the energy and spatial distributions of these particles in the Galactic center region from a kinetic equation. These particle distributions were then used to derive the characteristics of the main nuclear interaction gamma-ray lines.Results. Because the time period of star capture by the supermassive black hole is expected to be shorter than the lifetime of the ejected fast particles against Coulomb losses, the gamma-ray emission is predicted to be stationary. We find that the nuclear de-excitation lines should be emitted from a region with a maximum 5° angular radius. The total gamma-ray line flux below 8 MeV is calculated to be ̃ 10 -4 photons cm -2 s -1. The most promising lines for detection are those at 4.44 and ~6.2 MeV, with a predicted flux in each line of ̃10 -5 photons cm -2 s -1. Unfortunately, it is unlikely that this emission can be detected with the INTEGRAL observatory. But the predicted line intensities appear to be within reach of future gamma-ray space instruments. A future detection of de-excitation gamma-ray lines from the Galactic center region would provide unique information on the high-energy processes induced by the central supermassive black hole and the physical conditions of the emitting region. © 2009 ESO.en_HK
dc.languageengen_HK
dc.publisherE D P Sciences. The Journal's web site is located at http://www.aanda.orgen_HK
dc.relation.ispartofAstronomy and Astrophysicsen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectGalaxy: centeren_HK
dc.subjectGamma rays: theoryen_HK
dc.subjectRadiation mechanisms: non-thermalen_HK
dc.titleNuclear interaction gamma-ray lines from the Galactic center regionen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-6361&volume=508&issue=1&spage=1&epage=7&date=2009&atitle=Nuclear+interaction+gamma-ray+lines+from+the+galactic+center+regionen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1051/0004-6361/200911833en_HK
dc.identifier.scopuseid_2-s2.0-71849107527en_HK
dc.identifier.hkuros168771en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-71849107527&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume508en_HK
dc.identifier.issue1en_HK
dc.identifier.spage1en_HK
dc.identifier.epage7en_HK
dc.identifier.isiWOS:000272417700006-
dc.publisher.placeFranceen_HK
dc.identifier.scopusauthoridDogiel, VA=6603566238en_HK
dc.identifier.scopusauthoridTatischeff, V=8654848800en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridChernyshov, DO=14059433800en_HK
dc.identifier.scopusauthoridKo, CM=7202596730en_HK
dc.identifier.scopusauthoridIp, WH=26644885700en_HK

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