A Possible Origin of kHZ QPOs in Low-Mass X-ray Binaries

Abstract

A possible origin of kHz QPOs in low-mass X-ray binaries is proposed. Recent numerical MHD simulations of accretion disks with turbulent magnetic fields of MRI definitely show the presence of two-armed spiral structure in quasi-steady state of accretion disks. In such deformed disks, two-armed ($m=2$) c-mode ($n=1$) oscillations are excited by wave-wave resonant instability. Among these excited oscillations, the fundamental in the radial direction ($n_r=0$) will be the higher kHz QPO of a twin QPOs, and the first overtone ($n_r=1$) in the radial direction will be the lower kHz QPO of the twin. A possible cause of the twin high-frequency QPOs (HFQPOs) in BH X-ray binaries is also discussed.

arXiv comment20 pages, 6 figures; To be published in Publ. Aston. Soc. Japan, Vol. 72 (2020)

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Cited by in corpus (3)

• Simple analytic formula relating the mass and spin of accreting compact objects to their rapid X-ray variability
• Dynamics of charged particles and quasi-periodic oscillations in the vicinity of a distorted, deformed compact object embedded in a uniform magnetic field
• Oscillation properties of relativistic tori in the vicinity of a distorted deformed compact object