TY - JOUR
T1 - A possible origin of kilohertz quasi-periodic oscillations in low-mass X-ray binaries
AU - Kato, Shoji
AU - Machida, Mami
N1 - Funding Information:
We thank colleagues of M. Machida in the program of high-resolution numerical simulations of black hole accretion disks, T. Kawashima, Y. Kudoh, Y. Matsumoto, and R. Matsumoto, for allowing us to use their unpublished results before publication. This research used computational resources of the K computer provided by the RIKEN Advanced Institute for Computational Science through the HPCI System Research project (MM:Project ID:hp 180137, hp 190125). This work was supported by JSPS KAKENHI Grant Number 19K03916.
Publisher Copyright:
© 2020 The Author(s) 2020. Published by Oxford University Press on behalf of the Astronomical Society of Japan.
PY - 2020/6/1
Y1 - 2020/6/1
N2 - A possible origin of kilohertz quasi-periodic oscillations (QPOs) in low-mass X-ray binaries is proposed. Recent numerical magnetohydrodynamic simulations of accretion disks with turbulent magnetic fields of magneto-rotational instability definitely show the presence of two-Armed spiral structure in the 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 ($n{\rm r}=0$) will be the higher kHz QPO of twin QPOs, and the first overtone ($n{\rm r}=1$) in the radial direction will be the lower kHz QPO of the twin. A possible cause of the twin high-frequency QPOs in black hole X-ray binaries is also discussed in the final section.
AB - A possible origin of kilohertz quasi-periodic oscillations (QPOs) in low-mass X-ray binaries is proposed. Recent numerical magnetohydrodynamic simulations of accretion disks with turbulent magnetic fields of magneto-rotational instability definitely show the presence of two-Armed spiral structure in the 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 ($n{\rm r}=0$) will be the higher kHz QPO of twin QPOs, and the first overtone ($n{\rm r}=1$) in the radial direction will be the lower kHz QPO of the twin. A possible cause of the twin high-frequency QPOs in black hole X-ray binaries is also discussed in the final section.
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U2 - 10.1093/pasj/psaa019
DO - 10.1093/pasj/psaa019
M3 - Article
AN - SCOPUS:85089685416
SN - 0004-6264
VL - 72
JO - Publications of the Astronomical Society of Japan
JF - Publications of the Astronomical Society of Japan
IS - 3
M1 - 38
ER -