File Download
There are no files associated with this item.
Links for fulltext
(May Require Subscription)
- Publisher Website: 10.1143/JPSJS.78SA.133
- Scopus: eid_2-s2.0-66849084286
- WOS: WOS:000731108500026
- Find via
Supplementary
- Citations:
- Appears in Collections:
Conference Paper: Cosmic-ray production and x-ray and gamma-ray emission from the galactic center
Title | Cosmic-ray production and x-ray and gamma-ray emission from the galactic center |
---|---|
Authors | |
Keywords | Galactic Center Gamma-Rays X-Rays |
Issue Date | 2009 |
Publisher | Institute of Pure and Applied Physics. The Journal's web site is located at http://www.ipap.jp/jpsj/index.htm |
Citation | Journal of the Physical Society of Japan, 2009, v. 78 n. SUPPL. A, p. 133-137 How to Cite? |
Abstract | We assume that the energy source in the Galactic Center is the black hole Sgr A, which becomes active when a star is captured in a rate of ∼ 10-5yr-1. During the active phase relativistic protons with a characteristic energy ∼ 6 x 1052erg per capture are ejected. We suppose that the annihilation of secondary positrons produced by proton-proton collisions is observed as the 511 keV line flux from the Galactic bulge. Though these positron are generated with relatively high energies (> 30 MeV), our model satisfy the criterion derived by Beacom and Yiiksel based on the COMPTEL data in the range 1-30 MeV. From our estimations it follows also that a flux of gamma-ray de-excitation lines ∼ 2.5 x 10-5 ph cm-2 s-1 in the range below 8 MeV is produced by the relativistic protons in the Galactic center. A specific line is the one at 1.809 MeV from radioactivity of 26 Al. The predicted quasi-stationary flux of the 26Al 1.809 MeV line from the 1° x 1 central region is < 10-6 ph cm-2 s-1. We conclude also the the thermal 6.5 keV X-ray flux and the non-thermal hard X-ray flux in the range 14-40 keV observed by SUZAKU is emitted by subrelativistic protons produced by accretion processes. © 2009 The Physical Society of Japan. |
Persistent Identifier | http://hdl.handle.net/10722/176199 |
ISSN | 2023 Impact Factor: 1.5 2023 SCImago Journal Rankings: 0.612 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Dogiel, VA | en_US |
dc.contributor.author | Cheng, KS | en_US |
dc.contributor.author | Chernyshoy, DO | en_US |
dc.contributor.author | Tatisoheff, V | en_US |
dc.contributor.author | Ko, CM | en_US |
dc.contributor.author | Ip, WH | en_US |
dc.contributor.author | Kokubun, M | en_US |
dc.contributor.author | Maeda, Y | en_US |
dc.contributor.author | Mitsuda, K | en_US |
dc.date.accessioned | 2012-11-26T09:06:49Z | - |
dc.date.available | 2012-11-26T09:06:49Z | - |
dc.date.issued | 2009 | en_US |
dc.identifier.citation | Journal of the Physical Society of Japan, 2009, v. 78 n. SUPPL. A, p. 133-137 | - |
dc.identifier.issn | 0031-9015 | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/176199 | - |
dc.description.abstract | We assume that the energy source in the Galactic Center is the black hole Sgr A, which becomes active when a star is captured in a rate of ∼ 10-5yr-1. During the active phase relativistic protons with a characteristic energy ∼ 6 x 1052erg per capture are ejected. We suppose that the annihilation of secondary positrons produced by proton-proton collisions is observed as the 511 keV line flux from the Galactic bulge. Though these positron are generated with relatively high energies (> 30 MeV), our model satisfy the criterion derived by Beacom and Yiiksel based on the COMPTEL data in the range 1-30 MeV. From our estimations it follows also that a flux of gamma-ray de-excitation lines ∼ 2.5 x 10-5 ph cm-2 s-1 in the range below 8 MeV is produced by the relativistic protons in the Galactic center. A specific line is the one at 1.809 MeV from radioactivity of 26 Al. The predicted quasi-stationary flux of the 26Al 1.809 MeV line from the 1° x 1 central region is < 10-6 ph cm-2 s-1. We conclude also the the thermal 6.5 keV X-ray flux and the non-thermal hard X-ray flux in the range 14-40 keV observed by SUZAKU is emitted by subrelativistic protons produced by accretion processes. © 2009 The Physical Society of Japan. | en_US |
dc.language | eng | en_US |
dc.publisher | Institute of Pure and Applied Physics. The Journal's web site is located at http://www.ipap.jp/jpsj/index.htm | en_US |
dc.relation.ispartof | Journal of the Physical Society of Japan | en_US |
dc.subject | Galactic Center | en_US |
dc.subject | Gamma-Rays | en_US |
dc.subject | X-Rays | en_US |
dc.title | Cosmic-ray production and x-ray and gamma-ray emission from the galactic center | en_US |
dc.type | Conference_Paper | en_US |
dc.identifier.email | Cheng, KS: hrspksc@hkucc.hku.hk | en_US |
dc.identifier.authority | Cheng, KS=rp00675 | en_US |
dc.description.nature | link_to_subscribed_fulltext | en_US |
dc.identifier.doi | 10.1143/JPSJS.78SA.133 | - |
dc.identifier.scopus | eid_2-s2.0-66849084286 | en_US |
dc.identifier.hkuros | 241836 | - |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-66849084286&selection=ref&src=s&origin=recordpage | en_US |
dc.identifier.volume | 78 | en_US |
dc.identifier.issue | SUPPL. A | en_US |
dc.identifier.spage | 133 | en_US |
dc.identifier.epage | 137 | en_US |
dc.identifier.isi | WOS:000731108500026 | - |
dc.publisher.place | Japan | en_US |
dc.identifier.scopusauthorid | Dogiel, VA=6603566238 | en_US |
dc.identifier.scopusauthorid | Cheng, KS=9745798500 | en_US |
dc.identifier.scopusauthorid | Chernyshoy, DO=26644796600 | en_US |
dc.identifier.scopusauthorid | Tatisoheff, V=26645251300 | en_US |
dc.identifier.scopusauthorid | Ko, CM=7202596730 | en_US |
dc.identifier.scopusauthorid | Ip, WH=26644885700 | en_US |
dc.identifier.scopusauthorid | Kokubun, M=7006798464 | en_US |
dc.identifier.scopusauthorid | Maeda, Y=7402845669 | en_US |
dc.identifier.scopusauthorid | Mitsuda, K=7005132297 | en_US |
dc.identifier.issnl | 0031-9015 | - |