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AN MHD MODEL FOR MAGNETAR GIANT FLARES
Meng Y(蒙盈)1,2; Lin J(林隽)1; Zhang, L3; Reeves, KK4; Zhang QS(张钱生)1,5; Yuan, F6
Source PublicationASTROPHYSICAL JOURNAL
2014-04-10
Volume785Issue:1
DOI10.1088/0004-637X/785/1/62
Contribution Rank第1完成单位
Indexed BySCI
KeywordInstabilities Magnetic Reconnection Magnetohydrodynamics (Mhd) Stars: Flare Stars: Magnetic Field Stars: Neutron
Abstract

Giant flares on soft gamma-ray repeaters that are thought to take place on magnetars release enormous energy in a short time interval. Their power can be explained by catastrophic instabilities occurring in the magnetic field configuration and the subsequent magnetic reconnection. By analogy with the coronal mass ejection events on the Sun, we develop a theoretical model via an analytic approach for magnetar giant flares. In this model, the rotation and/or displacement of the crust causes the field to twist and deform, leading to flux rope formation in the magnetosphere and energy accumulation in the related configuration. When the energy and helicity stored in the configuration reach a threshold, the system loses its equilibrium, the flux rope is ejected outward in a catastrophic way, and magnetic reconnection helps the catastrophe develop to a plausible eruption. By taking SGR 1806-20 as an example, we calculate the free magnetic energy released in such an eruptive process and find that it is more than 10(47) erg, which is enough to power a giant flare. The released free magnetic energy is converted into radiative energy, kinetic energy, and gravitational energy of the flux rope. We calculated the light curves of the eruptive processes for the giant flares of SGR 1806-20, SGR 0526-66, and SGR 1900+14, and compared them with the observational data. The calculated light curves are in good agreement with the observed light curves of giant flares.

Funding ProjectProgram 973[2011CB811403] ; Program 973[2013CBA01503] ; NSFC[11273055] ; NSFC[11333007] ; NSFC[11121062] ; NSFC[11133005] ; CAS[KJCX2-EW-T07] ; CAS[XDB09000000] ; NSF[AGS-1156076]
Funding OrganizationProgram 973[2011CB811403, 2013CBA01503] ; NSFC[11273055, 11333007, 11121062, 11133005] ; CAS[KJCX2-EW-T07, XDB09000000] ; NSF[AGS-1156076]
Language英语
Subject Area天文学 ; 太阳与太阳系 ; 太阳物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
Archive Date2014-06-23
WOS IDWOS:000335639300062
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCORONAL MASS EJECTIONS ; CRUSTAL PLATE-TECTONICS ; SOFT GAMMA-REPEATERS ; X-RAY PULSAR ; FLUX-ROPE MODELS ; SOLAR ERUPTIONS ; NEUTRON-STARS ; SGR 1900+14 ; PARTICLE-ACCELERATION ; RADIATIVE MECHANISM
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6255
Collection太阳物理研究组
中国科学院天体结构与演化重点实验室
Corresponding AuthorMeng Y(蒙盈)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan 650011, China
2.University of Chinese Academy of Sciences, Beijing 100039, China
3.Department of Physics, Yunnan University, Kunming, Yunnan 650091, China
4.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
5.Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming, Yunnan 650011, China
6.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Meng Y,Lin J,Zhang, L,et al. AN MHD MODEL FOR MAGNETAR GIANT FLARES[J]. ASTROPHYSICAL JOURNAL,2014,785(1).
APA Meng Y,Lin J,Zhang, L,Reeves, KK,Zhang QS,&Yuan, F.(2014).AN MHD MODEL FOR MAGNETAR GIANT FLARES.ASTROPHYSICAL JOURNAL,785(1).
MLA Meng Y,et al."AN MHD MODEL FOR MAGNETAR GIANT FLARES".ASTROPHYSICAL JOURNAL 785.1(2014).
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