File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Fermi bubbles inflated by winds launched from the hot accretion flow in sgr a*

TitleFermi bubbles inflated by winds launched from the hot accretion flow in sgr a*
Authors
Keywordsaccretion, accretion disks
Issue Date2014
Citation
Astrophysical Journal, 2014, v. 790, n. 2 How to Cite?
AbstractA pair of giant gamma-ray Bubbles has been revealed by Fermi-LAT. In this paper we investigate their formation mechanism. Observations have indicated that the activity of the supermassive black hole located at the Galactic center, Sgr A*, was much stronger than at the present time. Specifically, one possibility is that while Sgr A* was also in the hot accretion regime, the accretion rate should be 103-104 times higher during the past ∼107 yr. On the other hand, recent magnetohydrodynamic numerical simulations of hot accretion flows have unambiguously shown the existence and obtained the properties of strong winds. Based on this knowledge, by performing three-dimensional hydrodynamical simulations, we show in this paper that the Fermi Bubbles could be inflated by winds launched from the "past" hot accretion flow in Sgr A*. In our model, the active phase of Sgr A* is required to last for about 10 million years and it was quenched no more than 0.2 million years ago. The central molecular zone (CMZ) is included and it collimates the wind orientation toward the Galactic poles. Viscosity suppresses the Rayleigh-Taylor and Kelvin-Helmholtz instabilities and results in the smoothness of the Bubbles edge. The main observational features of the Bubbles can be well explained. Specifically, the ROSAT X-ray features are interpreted by the shocked interstellar medium and the interaction region between the wind and CMZ gas. The thermal pressure and temperature obtained in our model are consistent with recent Suzaku observations. © 2014. The American Astronomical Society. All rights reserved..
Persistent Identifierhttp://hdl.handle.net/10722/226716
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorMou, Guobin-
dc.contributor.authorYuan, Feng-
dc.contributor.authorBu, Defu-
dc.contributor.authorSun, Mouyuan-
dc.contributor.authorSu, Meng-
dc.date.accessioned2016-06-29T01:58:23Z-
dc.date.available2016-06-29T01:58:23Z-
dc.date.issued2014-
dc.identifier.citationAstrophysical Journal, 2014, v. 790, n. 2-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/226716-
dc.description.abstractA pair of giant gamma-ray Bubbles has been revealed by Fermi-LAT. In this paper we investigate their formation mechanism. Observations have indicated that the activity of the supermassive black hole located at the Galactic center, Sgr A*, was much stronger than at the present time. Specifically, one possibility is that while Sgr A* was also in the hot accretion regime, the accretion rate should be 103-104 times higher during the past ∼107 yr. On the other hand, recent magnetohydrodynamic numerical simulations of hot accretion flows have unambiguously shown the existence and obtained the properties of strong winds. Based on this knowledge, by performing three-dimensional hydrodynamical simulations, we show in this paper that the Fermi Bubbles could be inflated by winds launched from the "past" hot accretion flow in Sgr A*. In our model, the active phase of Sgr A* is required to last for about 10 million years and it was quenched no more than 0.2 million years ago. The central molecular zone (CMZ) is included and it collimates the wind orientation toward the Galactic poles. Viscosity suppresses the Rayleigh-Taylor and Kelvin-Helmholtz instabilities and results in the smoothness of the Bubbles edge. The main observational features of the Bubbles can be well explained. Specifically, the ROSAT X-ray features are interpreted by the shocked interstellar medium and the interaction region between the wind and CMZ gas. The thermal pressure and temperature obtained in our model are consistent with recent Suzaku observations. © 2014. The American Astronomical Society. All rights reserved..-
dc.languageeng-
dc.relation.ispartofAstrophysical Journal-
dc.subjectaccretion, accretion disks-
dc.titleFermi bubbles inflated by winds launched from the hot accretion flow in sgr a*-
dc.typeArticle-
dc.description.natureLink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/790/2/109-
dc.identifier.scopuseid_2-s2.0-84904582425-
dc.identifier.volume790-
dc.identifier.issue2-
dc.identifier.spagenull-
dc.identifier.epagenull-
dc.identifier.eissn1538-4357-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats