A model for the upper kHz QPO coherence of an accreting neutron star

CORC > 高能物理研究所 > 中国科学院高能物理研究所 > 粒子天体物理中心

	A model for the upper kHz QPO coherence of an accreting neutron star
	Wang, J; Zhang, CM; Zhao, YH; Lin, YF; Yin, HX; Song, LM; Song LM(宋黎明)
刊名	ASTRONOMY & ASTROPHYSICS
	2011
卷号	528 页码:A126
关键词	accretion: accretion disks stars: neutron binaries: close X-rays: binaries
通讯作者	[Wang, J. ; Zhang, C. M. ; Zhao, Y. H.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China ; [Lin, Y. F.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China ; [Lin, Y. F.] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China ; [Yin, H. X.] Shandong Univ, Sch Space Sci & Phys, Weihai 264209, Peoples R China ; [Song, L. M.] Chinese Acad Sci, Inst High Energy Phys, Beijing 100049, Peoples R China
英文摘要	We investigate the coherence of the twin kilohertz quasi-periodic oscillations (kHz QPOs) in the low-mass X-ray binary (LMXB) theoretically. The profile of upper kHz QPO, interpreted as Keplerian frequency, is ascribed to the radial extent of the kHz QPO emission region associated with the transitional layer at the magnetosphere-disc boundary, which corresponds to the coherence of upper kHz QPO. The theoretical model for the Q-factor of upper kHz QPO is applied to the observational data of five Atoll and five Z sources, and the consistence is implied.
学科主题	Astronomy & Astrophysics
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
原文出处	SCI
语种	英语
WOS记录号	WOS:000288541600106
内容类型	期刊论文
源URL	[http://ir.ihep.ac.cn/handle/311005/241073]
专题	高能物理研究所_粒子天体物理中心
作者单位	中国科学院高能物理研究所
推荐引用方式 GB/T 7714	Wang, J,Zhang, CM,Zhao, YH,et al. A model for the upper kHz QPO coherence of an accreting neutron star[J]. ASTRONOMY & ASTROPHYSICS,2011,528:A126.
APA	Wang, J.,Zhang, CM.,Zhao, YH.,Lin, YF.,Yin, HX.,...&宋黎明.(2011).A model for the upper kHz QPO coherence of an accreting neutron star.ASTRONOMY & ASTROPHYSICS,528,A126.
MLA	Wang, J,et al."A model for the upper kHz QPO coherence of an accreting neutron star".ASTRONOMY & ASTROPHYSICS 528(2011):A126.