Full-transport radiation GRMHD simulations show super-Eddington black hole accretion is geometrically thick, drives strong outflows, and radiates with very low efficiency (below about 0.5% at 150 times Eddington).
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Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forests on summary statistics.
Of 21 megamaser-disk AGN, only NGC 4258 is resolvable on Earth-L2 baselines, and its spin-offset measurement is limited by 22 GHz maser astrometry, not by shadow centroid precision.
Large-scale magnetic polarity inversions in a SANE accretion flow, with non-thermal electrons, can reproduce Sgr A* near-infrared flares and the frequency-dependent radio time delays caused by plasma self-absorption.
Reconnection-powered inverse Compton emission with beaming along the upstream magnetic field can reproduce the flux and variability of M87*'s strongest very high energy flares.
JWST NIRCam infrared monitoring of Sgr A* finds fully continuous variability on seconds-to-year timescales, a faint/bright two-population flux distribution, and a 3-40 second lag of 4.8 micron behind 2.1 micron emission.
Sgr A*'s near-infrared spectral index is constant at α = −0.50 ± 0.08 ± 0.17 from 1 to 40 mJy, ruling out the synchrotron-cutoff-shift model of its variability.
A multiyear ALMA survey of 39 AGN and Sgr A* finds the Faraday rotation measure increases with frequency from 93 to 343 GHz, supporting magnetized jet sheaths while leaving accretion-flow screens possible.
In strongly magnetized proton-electron plasmas, 3D reconnection becomes less efficient at dissipating magnetic energy than 2D reconnection, opposite to the usual rule.
An inner magnetically arrested disk can form self-consistently in an advection-dominated accretion flow when the external magnetic field is strong, boosting jet power by about two orders of magnitude.
A new public GRMHD simulation library of MAD and SANE accretion flows across five black hole spins confirms SANE spin equilibrium near a*~0.94 and MAD jet-powered spin-down.
Adding separate electron thermodynamics and radiative cooling to magnetically arrested disk simulations of Sgr A* lowers predicted 230 GHz variability by nearly 50%, but still leaves it above observed levels.
Simulations of accreting black holes in standard and complex spacetimes indicate that magnetic geometry, quantum corrections, and binary dynamics influence flares, precession, photon rings, and multi-wavelength variability, with potential EHT constraints.
citing papers explorer
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Radiation GRMHD Models of Accretion onto Stellar-Mass Black Holes: I. Survey of Eddington Ratios
Full-transport radiation GRMHD simulations show super-Eddington black hole accretion is geometrically thick, drives strong outflows, and radiates with very low efficiency (below about 0.5% at 150 times Eddington).
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Identifying Observational Signatures of Flux Eruption Events in Supermassive Black Hole Accretion Flows with Machine Learning
Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forests on summary statistics.
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The Physical Origin and Time Lag of Multi-Frequency Flares from SgrA*
Large-scale magnetic polarity inversions in a SANE accretion flow, with non-thermal electrons, can reproduce Sgr A* near-infrared flares and the frequency-dependent radio time delays caused by plasma self-absorption.
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Modeling of lightcurves from reconnection-powered very high energy flares from M87*
Reconnection-powered inverse Compton emission with beaming along the upstream magnetic field can reproduce the flux and variability of M87*'s strongest very high energy flares.
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New Evidence for a Flux-independent Spectral Index of Sgr A* in the Near-infrared
Sgr A*'s near-infrared spectral index is constant at α = −0.50 ± 0.08 ± 0.17 from 1 to 40 mJy, ruling out the synchrotron-cutoff-shift model of its variability.
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Three-dimensional Dynamics of Strongly Magnetized Ion-Electron Relativistic Reconnection
In strongly magnetized proton-electron plasmas, 3D reconnection becomes less efficient at dissipating magnetic energy than 2D reconnection, opposite to the usual rule.
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Magnetic Flux Transport in Advection Dominated Accretion Flow Towards the Formation of Magnetically Arrested Disk
An inner magnetically arrested disk can form self-consistently in an advection-dominated accretion flow when the external magnetic field is strong, boosting jet power by about two orders of magnitude.
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A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
A new public GRMHD simulation library of MAD and SANE accretion flows across five black hole spins confirms SANE spin equilibrium near a*~0.94 and MAD jet-powered spin-down.
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Two-temperature treatments in magnetically arrested disk GRMHD simulations more accurately predict light curves of Sagittarius A*
Adding separate electron thermodynamics and radiative cooling to magnetically arrested disk simulations of Sgr A* lowers predicted 230 GHz variability by nearly 50%, but still leaves it above observed levels.
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GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex Spacetimes
Simulations of accreting black holes in standard and complex spacetimes indicate that magnetic geometry, quantum corrections, and binary dynamics influence flares, precession, photon rings, and multi-wavelength variability, with potential EHT constraints.