3D GRMHD collapsar simulations initialized with toroidal fields demonstrate that an accretion-disk dynamo generates poloidal fields and launches variable, wobbling jets with LGRB-comparable power.
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7 Pith papers cite this work. Polarity classification is still indexing.
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2026 7verdicts
UNVERDICTED 7representative citing papers
Magnetized disk models lower the thermal-viscous instability threshold to Eddington ratios of 0.01-0.03 and yield limit-cycle timescales of months to years, jointly matching observations in five CLAGN only when the inner disk is strongly magnetized.
Self-consistent spherical accretion simulations show cooling-enhanced growth of PBHs with radiative efficiency ~10^{-2} in the bremsstrahlung regime, yielding a critical seed mass of ~10^{-16} M_sun to consume a solar-mass star in a Hubble time.
Spectral fitting of 2022 observations indicates the disk reaches 7-17 R_g from the neutron star at low inclination, with first reported type-II bursts attributed to magnetospheric gating.
Requiring thermal stability and single-valuedness in the thin-disk Ṁ-Σ plane produces a viscosity law α(X) with X = P_gas/P_rad that eliminates the radiation-pressure dominated instability while preserving the effective-temperature profile.
Multi-wavelength data from SDSS J1430+2303 are interpreted as evidence that radiation pressure instabilities drive a shrinking unstable accretion-disk zone, based on timing analysis, weak soft excess, and SED-derived black-hole parameters.
Black hole spin constraints for Cyg X-1 from XRISM Resolve data are strongly model-dependent, ranging from a*~0.99 with relxill to a*~0 with relxillCp or reflkerrD.
citing papers explorer
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Jets from Scratch: A 3D Dynamo Origin of Long Gamma-Ray Burst Jets
3D GRMHD collapsar simulations initialized with toroidal fields demonstrate that an accretion-disk dynamo generates poloidal fields and launches variable, wobbling jets with LGRB-comparable power.
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A magnetically-supported disk-corona model for Changing-Look AGN transitions
Magnetized disk models lower the thermal-viscous instability threshold to Eddington ratios of 0.01-0.03 and yield limit-cycle timescales of months to years, jointly matching observations in five CLAGN only when the inner disk is strongly magnetized.
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Accretion of Primordial Black Holes in Stellar Interiors
Self-consistent spherical accretion simulations show cooling-enhanced growth of PBHs with radiative efficiency ~10^{-2} in the bremsstrahlung regime, yielding a critical seed mass of ~10^{-16} M_sun to consume a solar-mass star in a Hubble time.
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On the assessment of the disk truncation and detection of type-II bursts from the accreting millisecond X-ray Pulsar IGR J17062-6143
Spectral fitting of 2022 observations indicates the disk reaches 7-17 R_g from the neutron star at low inclination, with first reported type-II bursts attributed to magnetospheric gating.
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Radiation-pressure instability is an artifact of constant-$\alpha$ closure
Requiring thermal stability and single-valuedness in the thin-disk Ṁ-Σ plane produces a viscosity law α(X) with X = P_gas/P_rad that eliminates the radiation-pressure dominated instability while preserving the effective-temperature profile.
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Radiation Pressure Instability in the "turn-on" Changing-Look AGN SDSS J1430+2303
Multi-wavelength data from SDSS J1430+2303 are interpreted as evidence that radiation pressure instabilities drive a shrinking unstable accretion-disk zone, based on timing analysis, weak soft excess, and SED-derived black-hole parameters.
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Model dependence of XRISM black-hole spin constraints in Cyg X-1
Black hole spin constraints for Cyg X-1 from XRISM Resolve data are strongly model-dependent, ranging from a*~0.99 with relxill to a*~0 with relxillCp or reflkerrD.