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Two-dimensional magnetohydrodynamics simulations of young Type Ia supernova remnants
Fang, Jun1,2; Zhang, Li1
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2012-08
Volume424Issue:4Pages:2811-2820
DOI10.1111/j.1365-2966.2012.21405.x
Indexed BySCI
KeywordInstabilities Mhd Ism: Supernova Remnants
Abstract

Using two-dimensional magnetohydrodynamics (MHD) simulations, we investigate the dynamical properties of Type Ia supernova remnants (SNRs) evolved either in a uniform ambient medium or from an interaction with a dense clump. The initial conditions assume that the expansion of the supernova ejecta is of free inertia with a power-law density distribution in the outer part of the ejecta. To include the effects of the diffusive shock acceleration process and the escape of the accelerated particles from the shock front, we use different adiabatic indices in the simulations to study the dynamical evolution of the Type Ia SNRs. Moreover, we investigate the interactions of a SNR with either a small or a large clump. A double-shock structure with a contact discontinuity is produced as the ejecta flow supersonically in the ambient medium; RayleighTaylor instability is clearly shown as fingers near the contact discontinuity in the contour maps of density, and a high density and a high magnetic field can be triggered because of the instability around the RayleighTaylor fingers. We perform simulations with different adiabatic indices, and the results show that a narrower intershock region is produced with a smaller adiabatic index because a larger compression ratio for the SNR shock is induced. The influence of the RayleighTaylor instability on the morphologies of both the forward and reverse shocks is more significant with a smaller adiabatic index. Finally, the simulations of a SNR interacting with a dense clump show that the morphology of the remnant is greatly twisted after the collision, and a filament with a high density and a high magnetic field can be produced as a SNR colliding with a large dense clump.

Funding ProjectNational Natural Science Foundation of China[NSFC 11103016] ; National Natural Science Foundation of China[11173020] ; 973 Programme[2009CB824800] ; Yunnan Province[2011FB012] ; Foundation of Yunnan University[21132014] ; Foundation of Yunnan University[2010YB043] ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[OP201101]
Funding OrganizationNational Natural Science Foundation of China[NSFC 11103016,11173020] ; 973 Programme[2009CB824800] ; Yunnan Province[2011FB012] ; Foundation of Yunnan University[21132014, 2010YB043] ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences[OP201101]
Language英语
Subject Area天文学 ; 恒星与银河系
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherWILEY-BLACKWELL
Publication Place111 RIVER ST, HOBOKEN 07030-5774, NJ USA
ISSN0035-8711
URL查看原文
WOS IDWOS:000307385100033
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordNONLINEAR SHOCK ACCELERATION ; RAYLEIGH-TAYLOR INSTABILITIES ; PARTICLE-ACCELERATION ; MAGNETIC-FIELD ; SN 1006 ; EMISSION ; TURBULENT ; EVOLUTION ; EJECTA ; WAVES
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9429
Collection中国科学院天体结构与演化重点实验室
Corresponding AuthorFang, Jun
Affiliation1.Department of Physics, Yunnan University, Kunming, China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
Recommended Citation
GB/T 7714
Fang, Jun,Zhang, Li. Two-dimensional magnetohydrodynamics simulations of young Type Ia supernova remnants[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2012,424(4):2811-2820.
APA Fang, Jun,&Zhang, Li.(2012).Two-dimensional magnetohydrodynamics simulations of young Type Ia supernova remnants.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,424(4),2811-2820.
MLA Fang, Jun,et al."Two-dimensional magnetohydrodynamics simulations of young Type Ia supernova remnants".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 424.4(2012):2811-2820.
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