2006/11/30 by Ding-Xiong Wang, Ding‐Xiong Wang, Yong-Chun Ye +3 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #astro-ph
paper · pdf · doi:10.1086/511067
published as Astrophys.J.657:428-435,2007 · 17 pages, 6 figures, accepted by APJ
arxiv created 2007/01/30 · openalex publication_date 2007/03/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We argue, following our earlier works (the "CEBZMC model"), that the phenomenon of twin-peak high-frequency quasi-periodic oscillations (QPOs) observed in black hole X-ray binaries is caused by magnetic coupling (MC) between the accretion disk and the black hole (BH). Due to MC, two bright spots occur at separate radial locations r in and r out at the disk surface, energized by a kind of Blandford-Znajek mechanism (BZ). We assume, following the Kluzniak-Abramowicz QPO resonance model, that the Keplerian frequencies at these two locations are in the 3 : 2 ratio. With this assumption, we estimate the BH spins in several sources, including GRO J1655-40, GRS 1915+105, XTE J1550-564, H1743-322, and Sgr A*. We give an interpretation of the "jet line" in the hardness-intensity plane, discussing the parameter space consisting of the BH spin and the power-law index for the variation of the large-scale magnetic field in the disk. Furthermore, we propose a new scenario for the spectral state transitions in BH X-ray binaries based on fluctuations in the densities of the accreting plasma from a companion star.