GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex Spacetimes

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Original abstract

This dissertation studies the electromagnetic signatures of accreting supermassive black holes using general relativistic magnetohydrodynamic simulations and covariant radiative-transfer calculations. It develops a unified numerical framework for modeling black-hole accretion, jet launching, flaring activity, and multi-band variability in Kerr, non-Kerr, and binary black-hole spacetimes. For isolated Kerr black holes, I investigate how magnetic-field geometry affects accretion dynamics and transient emission. Multi-loop magnetic configurations naturally produce reconnection events and flux-rope structures that can power near-infrared flares from Sagittarius A*, while the evolving optical depth of expanding plasma explains delayed millimeter emission. I also show that in tilted magnetically arrested disks, magnetic torques can drive retrograde disk and jet precession. The dissertation then applies the same framework to more complex spacetimes. Simulations of accretion onto regular loop-quantum black holes show that quantum-gravity corrections can modify photon-ring size, polarization structure, and jet power, leading to observational constraints from Event Horizon Telescope data. Finally, simulations of supermassive binary black holes in time-dependent spacetimes reveal how gravitational self-lensing, shock activity, and spin-orbit coupling shape multi-wavelength light curves and jet precession. Together, these results connect relativistic plasma dynamics with current and future observations of black-hole systems.

Links and sources

• Official / arXiv page
• PDF from original source

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