The emission positions of kHz QPOs and Kerr spacetime influence

作     者：ZHANG ChengMin1,WEI YingChun1,YIN HongXing1,ZHAO YongHeng1,LEI YaJuan2,SONG LiMing2,ZHANG Fan2 & YAN Yan3 1 National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100012,China 2 Institute of High Energy Physics,Chinese Academy of Sciences,19B Yuquan Road,Beijing 100049,China 3 Urumqi Observatory,National Astronomical Observatories,CAS,Urumqi 830011,China 

作者机构：National Astronomical Observatories Chinese Academy of Sciences Beijing China Institute of High Energy Physics Chinese Academy of Sciences Beijing China Urumqi Observatory National Astronomical Observatories CAS Urumqi China 

出 版 物：《Science China(Physics,Mechanics & Astronomy)》 (中国科学：物理学、力学、天文学（英文版）)

年 卷 期：2010年第53卷第S1期

页      面：114-116页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 0702[理学-物理学] 

基　　金：supported by the National Basic Research Program of China (Grant No. 2009CB824800) the National Natural Science Foundation of China (Grant No. 10773017) 

主　　题：kHz QPO neutron star low-mass X-ray binaries 

摘      要：Based the Alfven wave oscillation model(AWOM) and relativistic precession model(RPM) for twin kHz QPOs,we estimate the emission positions of most detected kHz QPOs to be at r=18+/-3 km(R/15 km),except Cir X-1 at r-30+/-5 km(R/15 km).For the proposed Keplerian frequency as an upper limit to kHz QPO,the spin effects in Kerr Spacetime are discussed,which have about a 5%(2%) modification for that of the Schwarzchild case for the spin frequency of 1000(400) *** application to the four typical QPO sources,Cir X-1,Sco X-1,SAX J1808.4-3658 and XTE 1807-294,is mentioned.