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Spectral fits to M87 core data from radio to hard x-ray are generated via aspecially selected software suite, comprised of the HARM GRMHD accretion diskmodel and a 2D Monte Carlo radiation transport code. By determining appropriateparameter changes necessary to fit x-ray quiescent and flaring behavior ofM87's core, we assess the reasonableness of various flaring mechanisms. Thisshows that an accretion disk model of M87's core out to 28 GM/c^2 can describethe inner emissions. High spin rates show GRMHD-driven polar outflowgeneration, without citing an external jet model. Our results favor accretionrate changes as the dominant mechanism of x-ray flux and index changes, withvariations in density of approximately 20% necessary to scale between theaverage x-ray spectrum and flaring or quiescent spectra. The best fitparameters 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 aradiative efficiency eta = 0.1). These results demonstrate that the immediatesurroundings of M87's core are appropriate to explain observed x-rayvariability.

Numerical Modeling of Multi-wavelength Spectra of M87 Core Emission