Numerical Modeling of Multi-wavelength Spectra of M87 Core Emission

Abstract

Spectral fits to M87 core data from radio to hard x-ray are generated via a specially selected software suite, comprised of the HARM GRMHD accretion disk model and a 2D Monte Carlo radiation transport code. By determining appropriate parameter changes necessary to fit x-ray quiescent and flaring behavior of M87's core, we assess the reasonableness of various flaring mechanisms. This shows that an accretion disk model of M87's core out to 28 GM/c^2 can describe the inner emissions. High spin rates show GRMHD-driven polar outflow generation, without citing an external jet model. Our results favor accretion rate changes as the dominant mechanism of x-ray flux and index changes, with variations in density of approximately 20% necessary to scale between the average x-ray spectrum and flaring or quiescent spectra. The best fit parameters are black hole spin a/M > 0.8 and maximum accretion flow density n <= 3x10^7 cm^-3, equivalent to horizon accretion rates between m_dot = M_dot/M_dot_Edd ~ 2x10^-6 and 1x10^-5 (with M_dot_Edd defined assuming a radiative efficiency eta = 0.1). These results demonstrate that the immediate surroundings of M87's core are appropriate to explain observed x-ray variability.

Accepted for publication in the Astrophysical Journal

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Cited by in corpus (6)

• General relativistic magnetohydrodynamical simulations of the jet in M87
• General relativistic magnetohydrodynamical $\kappa$-jet models for Sgr A*
• Probing the central black hole in M87 with gamma-rays
• Black hole spin from wobbling and rotation of the M87 jet and a sign of a magnetically arrested disc
• Do Intermediate-Mass Black Holes Exist in Globular Clusters?
• Disk evolution of the M87's nucleus observed in 2008