Evolution of QPOs in GX 339-4 and EXO 1846-031 with Insight-HXMT and NICER
Zuobin ZhangCenter for Astronomy and Astrophysics, Center for Field Theory and Particle Physics, and Department of Physics, Fudan University, Shanghai 200438, ChinaH. LiuCenter for Astronomy and Astrophysics, Center for Field Theory and Particle Physics, and Department of Physics, Fudan University, Shanghai 200438, ChinaDivya RawatObservatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS, F-67000 Strasbourg, FranceCosimo BambiSchool of Natural Sciences and Humanities, New Uzbekistan University, Tashkent 100007, UzbekistanRanjeev MisraInter-University Center for Astronomy and Astrophysics, Ganeshkhind, Pune 411007, IndiaPengju WangKey Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, ChinaLong JiSchool of Physics and Astronomy, Sun Yat-Sen University, Zhuhai 519082, ChinaShu ZhangKey Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, ChinaShuang‐Nan ZhangUniversity of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
ABI
Аннотация
We conduct a spectral and timing analysis of GX 339-4 and EXO 1846-031 with the aim of studying the evolution of Type-C QPOs with spectral parameters. The high cadence data from Insight-HXMT and NICER allow us to track them. Type-C QPOs appear at the end of low-hard state and/or hard-intermediate state. The results reveal that the QPO frequency is closely related to the inner disk radius and mass accretion rate in the two sources. Such a correlation is nicely consistent with the dynamic frequency model.
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Показатели — AkademScholar · Скоро