Fe Kα lines from accreting black holes are produced mostly outside 10 gravitational radii due to radial ionization gradients, allowing broad profiles without high spin.
Disk Emission from Magneto-hydrodynamic Simulations of Spinning Black Holes
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We present the results of a new series of global 3D relativistic magneto-hydrodynamic (MHD) simulations of thin accretion disks around spinning black holes. The disks have aspect ratios of $H/R\sim 0.05$ and spin parameters $a/M=0, 0.5, 0.9$, and $0.99$. Using the ray-tracing code Pandurata, we generate broad-band thermal spectra and polarization signatures from the MHD simulations. We find that the simulated spectra can be well fit with a simple, universal emissivity profile that better reproduces the behavior of the emission from the inner disk, compared to traditional analyses carried out using a Novikov-Thorne thin disk model. Lastly, we show how spectropolarization observations can be used to convincingly break the spin-inclination degeneracy well-known to the continuum fitting method of measuring black hole spin.
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astro-ph.HE 2years
2026 2representative citing papers
Spins of low-mass AGN black holes decrease with mass, supporting mergers or chaotic accretion as growth mechanisms and suggesting an evolutionary sequence where spins first decrease then slowly increase.
citing papers explorer
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Simulation-Based Prediction of Black Hole Fe K$\alpha$ Line Profiles
Fe Kα lines from accreting black holes are produced mostly outside 10 gravitational radii due to radial ionization gradients, allowing broad profiles without high spin.
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Estimation of black hole spins in low-mass AGNs and comparison with other types of AGNs
Spins of low-mass AGN black holes decrease with mass, supporting mergers or chaotic accretion as growth mechanisms and suggesting an evolutionary sequence where spins first decrease then slowly increase.