A magnetic reconnection model for quasi-periodic oscillations in black hole systems

Abstract

The quasi-periodic oscillations (QPOs) in black hole (BH) systems of different scales are interpreted based on the magnetic reconnection of the large-scale magnetic fields generated by the toroidal electric currents flowing in the inner region of accretion disk, where the current density is assumed to be proportional to the mass density of the accreting plasma. The magnetic connection (MC) is taken into account in resolving the dynamic equations of the accretion disk, in which the MC between the inner and outer disk regions, the MC between the plunging region and the disk, and the MC between the BH horizon and the disk are involved. It turns out that the single QPO frequency of several BH systems of different scales can be fitted by invoking the magnetic reconnection due to the MC between the inner and outer regions of the disk, where the BH binaries XTE J1859+226, XTE J1650-500 and GRS 1915+105 and the massive BHs in NGC 5408 X-1 and RE J1034+396 are included. In addition, the X-ray spectra corresponding to the QPOs are fitted for these sources based on the typical disk-corona model.

13 pages, 10 figures, accepted for publication in RAA

References in corpus (4)

• X-ray Properties of Black-Hole Binaries
• The hard X-ray spectral evolution in X-ray binaries and its application to constrain the black hole mass of ultraluminous X-ray sources
• A Model of Magnetically Induced Disc-Corona for Black Hole Binaries
• Effects of Magnetic Coupling on Radiation from Accretion Disc around a Kerr Black Hole

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