Self-gravity in collapsar models produces temporary jet quenching, narrower jets, and modified timescales compared to non-self-gravitating cases, potentially explaining GRB variability and failed bursts.
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Radiative cooling in two-temperature GRMHD simulations for M87* produces cooler inner disks, dimmer disks, brighter and more extended jets, and lower total flux at 230 GHz compared to non-cooling models.
Flux eruptions in MADs enhance non-axisymmetry near the black hole via m=1 and m=2 modes driven by vertical magnetic flux bundles formed through reconnection and expelled by buoyancy.
Radiative cooling thins hot accretion disks around black holes, reduces wind power, and makes inflow-rate decrease depend more on MRI-driven turbulence than on winds as cooling strengthens.
Spectral index maps of the limb-brightened jet in 3C 84 show significant evolution across three epochs, indicating dynamic filamentary structures, evolving magnetic fields, and interaction with the ambient medium.
citing papers explorer
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Three-dimensional GRMHD simulations of jet formation and propagation in self-gravitating collapsing stars
Self-gravity in collapsar models produces temporary jet quenching, narrower jets, and modified timescales compared to non-self-gravitating cases, potentially explaining GRB variability and failed bursts.
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Impacts of radiative cooling on the images of a black hole shadow and extended jets in two-temperature GRMHD simulations
Radiative cooling in two-temperature GRMHD simulations for M87* produces cooler inner disks, dimmer disks, brighter and more extended jets, and lower total flux at 230 GHz compared to non-cooling models.
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The azimuthal structure of magnetically arrested disks during flux eruption events
Flux eruptions in MADs enhance non-axisymmetry near the black hole via m=1 and m=2 modes driven by vertical magnetic flux bundles formed through reconnection and expelled by buoyancy.
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Radiative cooling effects on black hole hot accretion flows around the sub-Bondi radius
Radiative cooling thins hot accretion disks around black holes, reduces wind power, and makes inflow-rate decrease depend more on MRI-driven turbulence than on winds as cooling strengthens.
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Spectral index evolution of the limb-brightened jet in 3C 84
Spectral index maps of the limb-brightened jet in 3C 84 show significant evolution across three epochs, indicating dynamic filamentary structures, evolving magnetic fields, and interaction with the ambient medium.