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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Pair production via radiative magnetic reconnection near spinning black holes supplies non-uniform plasma to jets at levels sufficient to explain M87 radio emission.
Derives B*(d) and N*(d) for AGN jet cores from self-absorbed synchrotron emission model with power-law assumptions on Doppler factor, Lorentz factor, B, and N versus jet width d.
Numerical simulations show Shannon entropy and MIPP indicators distinguish chaotic from regular orbits of charged particles near weakly magnetized black holes in Einstein-ModMax theory, with parameters restricted by EHT shadow observations.
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.
Synthetic EHT data from semi-analytic jet models show that the 2022 array configuration enables robust recovery of faint horizon-scale jet emission in M87* when jet intensity exceeds a determined lower limit.
GRRT simulations show that raising the dilaton parameter shrinks the bright ring while increasing its width and brightness, disk thickness reduces diameter and width with weaker brightness impact, and both affect allowed ranges versus EHT Sgr A* data and the polarization coefficient beta2.
Multi-component galactic potentials strongly shift critical points, shock parameters, and acoustic surface gravity in transonic accretion flows around non-rotating pseudo-Schwarzschild black holes under the vertical equilibrium model.
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