GRMHD and GRRT simulations of accretion onto a spinning Kerr-like wormhole show throat-dominated emission producing quasi-periodic modulations in 230 GHz light curves, distinct from Kerr black holes.
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Automatic-differentiation image sensitivities from GRMHD snapshots enable gradient-based recovery of inclination and electron-heating parameters under idealized, blurred, and noisy conditions.
A Chimera accretion flow can sustain MAD-level horizon flux and electromagnetic jet power without the standard MAD's eruptive variability, mass-flow geometry, or inner-disk morphology, so MAD-like behavior is multi-diagnostic and history-dependent.
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.
RIAF polarized-transfer models of six poloidal field geometries show Faraday-conversion-dominated, polarity-invariant CP for radial/parabolic fields and emission-dominated, polarity-sensitive CP for dipole/vertical fields; ALMA’s negative V_net excludes reversed fields at high inclination.
GRMHD models show PA1 aligns with the approaching limb for high spins, enabling mild disfavoring of low spins and strong disfavoring of Earth-pointing spins in M87* from EHT data, with similar potential for Sgr A*.
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.
GRMHD simulations at spins 0.9375 and 0.998 yield similar fluid properties and full-Stokes EHT images, indicating prior lower-spin runs remain representative for a ≳ 0.9375.
GPUmonty delivers a 12x speedup over grmonty by parallelizing superphoton operations on GPUs while keeping errors below 1% in tests against analytic solutions and prior codes.
citing papers explorer
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Dynamics and Radiative Signatures of Accretion Flows onto a Kerr-like Wormhole
GRMHD and GRRT simulations of accretion onto a spinning Kerr-like wormhole show throat-dominated emission producing quasi-periodic modulations in 230 GHz light curves, distinct from Kerr black holes.
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Sensitivities of Black Hole Images from GRMHD Simulations
Automatic-differentiation image sensitivities from GRMHD snapshots enable gradient-based recovery of inclination and electron-heating parameters under idealized, blurred, and noisy conditions.
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The SANE, the MAD, and the Chimera
A Chimera accretion flow can sustain MAD-level horizon flux and electromagnetic jet power without the standard MAD's eruptive variability, mass-flow geometry, or inner-disk morphology, so MAD-like behavior is multi-diagnostic and history-dependent.
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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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Circular polarization images of Sgr A* for different magnetic field geometries
RIAF polarized-transfer models of six poloidal field geometries show Faraday-conversion-dominated, polarity-invariant CP for radial/parabolic fields and emission-dominated, polarity-sensitive CP for dipole/vertical fields; ALMA’s negative V_net excludes reversed fields at high inclination.
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Ring Position Angles and Spin in M87* and Sgr A*
GRMHD models show PA1 aligns with the approaching limb for high spins, enabling mild disfavoring of low spins and strong disfavoring of Earth-pointing spins in M87* from EHT data, with similar potential for Sgr A*.
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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.
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Observational Properties of Near-Maximally Spinning Supermassive Black Holes
GRMHD simulations at spins 0.9375 and 0.998 yield similar fluid properties and full-Stokes EHT images, indicating prior lower-spin runs remain representative for a ≳ 0.9375.
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$\texttt{GPUmonty}$: A GPU-accelerated relativistic Monte Carlo radiative transfer code
GPUmonty delivers a 12x speedup over grmonty by parallelizing superphoton operations on GPUs while keeping errors below 1% in tests against analytic solutions and prior codes.