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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MIST provides a new publicly available grid of solar-scaled stellar isochrones and evolutionary tracks computed self-consistently with MESA from pre-main sequence through advanced stages for masses 0.1-300 solar masses and metallicities -2 to 0.5.
Tayler-Spruit magnetic fields can convert low-frequency internal gravity waves to magneto-gravity waves in low-mass star cores, with effects strongest on the red giant branch in central regions.
MESA Star has been substantially updated with new capabilities for low-mass giant planets, asteroseismology coupling, rotating star models, and uninterrupted massive star evolution to core collapse.
Rotating stellar models initialized with observed velocity distributions yield modestly lower initial mass estimates for SN II progenitors than non-rotating models, with an upper limit of 20.4 solar masses.
MESA gains simultaneous binary star evolution, large nuclear networks, implicit hydrodynamics, and GYRE pulsation coupling for better massive star and supernova modeling.
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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MESA Isochrones and Stellar Tracks (MIST). I: Solar-Scaled Models
MIST provides a new publicly available grid of solar-scaled stellar isochrones and evolutionary tracks computed self-consistently with MESA from pre-main sequence through advanced stages for masses 0.1-300 solar masses and metallicities -2 to 0.5.
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Co-existence of Internal Gravity Waves and Tayler-Spruit Magnetic Fields in the Radiative Core of Low-mass Stars
Tayler-Spruit magnetic fields can convert low-frequency internal gravity waves to magneto-gravity waves in low-mass star cores, with effects strongest on the red giant branch in central regions.
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Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
MESA Star has been substantially updated with new capabilities for low-mass giant planets, asteroseismology coupling, rotating star models, and uninterrupted massive star evolution to core collapse.
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Impact of stellar rotation on type II supernova progenitor masses from pre-explosion imaging
Rotating stellar models initialized with observed velocity distributions yield modestly lower initial mass estimates for SN II progenitors than non-rotating models, with an upper limit of 20.4 solar masses.
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Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
MESA gains simultaneous binary star evolution, large nuclear networks, implicit hydrodynamics, and GYRE pulsation coupling for better massive star and supernova modeling.