Correlation between 3:2 QPO pairs and Jets in Black Hole X-ray Binaries

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dc.creatorWang, Ding-Xiong
dc.creatorYe, Yong-Chun
dc.creatorHuang, Chang-Yin
dc.date2006-11-18
dc.date2007-01-30
dc.date.accessioned2026-07-07T10:20:54Z
dc.date.available2026-07-07T10:20:54Z
dc.descriptionWe 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 accretion disk and black hole (BH). Due to MC, two bright spots occur at two separate radial locations r_{in} and r_{out} at the disk surface, energized by a kind of the Blandford-Znajek mechanism (BZ). We assume, following the Kluzniak-Abramowicz QPO resonance model, that 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 fluctuation in densities of accreting plasma from a companion star.
dc.description17 pages, 6 figures, accepted by APJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0611592
dc.identifierhttp://arxiv.org/abs/astro-ph/0611592
dc.identifierAstrophys.J.657:428-435,2007
dc.identifierdoi:10.1086/511067
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/174997
dc.subjectAstrophysics
dc.titleCorrelation between 3:2 QPO pairs and Jets in Black Hole X-ray Binaries
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