Effects of resistivity on standing shocks in low angular momentum flows around black holes

Abstract

We study two dimensional low angular momentum flow around the black hole using the resistive magnetohydrodynamic module of PLUTO code. Simulations have been performed for the flows with parameters of specific angular momentum, specific energy, and magnetic field which may be expected for the flow around Sgr A*. For flows with lower resistivity $\eta =10^{-6}$ and $0.01$, the luminosity and the shock location on the equator vary quasi-periodically. The power density spectra of luminosity variation show the peak frequencies which correspond to the periods of $5\times 10^5$, $1.4\times 10^5$, and $5\times 10^4$ seconds, respectively. These quasi-periodic oscillations (QPOs) occur due to the interaction between the outer oscillating standing shock and the inner weak shocks occurring at the innermost hot blob. While for cases with higher resistivity $\eta =0.1$ and 1.0, the high resistivity considerably suppresses the magnetic activity such as the MHD turbulence and the flows tend to be steady and symmetric to the equator. The steady standing shock is formed more outward compared with the hydrodynamical flow. The low angular momentum flow model with the above flow parameters and with low resistivity has a possibility for the explanation of the long-term flares with $\sim$ one per day and $\sim 5-10$ days of Sgr A* in the latest observations by Chandra, Swift, and XMM-Newton monitoring of Sgr A*.

arXiv comment14 pages, 9 figures, Accepted for publication in the Research in Astronomy and Astrophysics journal

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Cited by in corpus (4)

• Three Dimensional Simulations of Advective, Sub-Keplerian Accretion Flow onto Non-rotating Black Holes
• Radiative shock oscillation model for the long-term flares of Sgr A*
• Truncated accretion discs in black hole X-ray binaries: dynamics and variability signatures
• Time delays between radio and X-ray and between narrow radio bands of Sgr A* flares in the shock oscillation model