Low-frequency, one-armed oscillations in black hole accretion flows obtained from direct 3D MHD simulations

Details Low-frequency, one-armed oscillations in black hole accretion flows obtained from direct 3D MHD simulations Low-frequency, one-armed oscillations in black hole accretion flows obtained from direct 3D MHD simulations

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..405m&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Computer Science

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We present the results of global 3D simulation of optically thin black hole accretion flow. The initial disk has a sub Keplerian angular momentum. The disk is assumed to be threaded by weak (beta=100) toroidal magnetic field where beta is the ratio of gas pressure to magnetic pressure. The sound speed of the initial disk is about 0.006c. The initial disk is assumed to be embedded in a low density, spherical, isothermal halo. General relativistic effects are simulated by using the pseudo-Newtonian potential. The magnetic fields are amplified due to the magneto-rotational instability and saturates when beta ˜10. When the temperature is low enough, since Maxwell stress becomes small (alpha<0.01), inner torus is created around 4-10 R[g] where R[g] is the Schwarzschild radius, because matter accumulates. This inner torus shows the m=1, one-armed density distribution with the vertical oscillation (Kato et al. 1998). The oscillation period is about 0.1s when we assume 10 solar mass black hole. This frequency agrees with the low-frequency QPOs observed in low/hard state. The disk ejects wind whose opening angle is about 30 degree. The propagation speed of the wind is about 0.05c. The disk wind shows fluctuations with frequency about 60 Hz. In this presentation, we will show the structure of the wind and discuss how the wind modifies the image of the black hole SgrA*, a target of the VSOP-2.

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