3D MHD simulations of pre-supernova Wolf-Rayet progenitors reveal cylindrical rotation and amplified small-scale magnetic fields that connect regions isolated in 1D models.
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Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.
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.
3D MHD simulations of pre-supernova progenitors find turbulent mixing in oxygen and silicon shells deviates from standard 1D mixing-length prescriptions, with proposed updates for stellar evolution codes.
Simulations find nested bow shocks around an engulfed neutron star enhance drag force 10-100 times over Bondi-Hoyle-Lyttleton and allow force reversal based on envelope conditions.
Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.
Multi-D progenitor perturbations leave shock revival and explosion energetics essentially unchanged in 2D CHIMERA runs; any effects sit below the level of numerical stochasticity.
The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.
New MESA stellar tracks with varied winds and convective mixing produce a primary black hole mass function with twin peaks near 8 and 13 solar masses in most variations, the higher peak dominated by mass-ratio-reversal systems, with rates varying by a factor of six.
Failed common envelope mergers yield 6-14 solar mass stripped stars consistent with long-lived core He-burning objects that appear single or in wide binaries from hierarchical triples.
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.
citing papers explorer
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The first 3D MHD core-collapse progenitors II: Rotation, magnetic-field amplification, and magnetic topology
3D MHD simulations of pre-supernova Wolf-Rayet progenitors reveal cylindrical rotation and amplified small-scale magnetic fields that connect regions isolated in 1D models.
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Observational signatures of thermonuclear electron-capture supernovae -- Ne II line strengthening and color evolution as traces of the explosion mechanism
Synthetic observables from tECSN models show slower early red-color decline due to higher Ti/Cr and a late-time 12.8 μm Ne II line that strengthens over time, unlike comparable CO deflagration models.
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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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The first 3D MHD core-collapse progenitors I: General properties, convection and nuclear burning
3D MHD simulations of pre-supernova progenitors find turbulent mixing in oxygen and silicon shells deviates from standard 1D mixing-length prescriptions, with proposed updates for stellar evolution codes.
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Numerical Studies of Accretion Flows onto a Neutron Star Engulfed in a Massive Star
Simulations find nested bow shocks around an engulfed neutron star enhance drag force 10-100 times over Bondi-Hoyle-Lyttleton and allow force reversal based on envelope conditions.
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A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors
Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.
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Impacts of Multidimensional Progenitor Perturbations on Core-Collapse Supernova Explosions
Multi-D progenitor perturbations leave shock revival and explosion energetics essentially unchanged in 2D CHIMERA runs; any effects sit below the level of numerical stochasticity.
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The location of the upper edge of the pair-instability supernovae black hole mass gap
The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.
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Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with COSMIC-METISSE
New MESA stellar tracks with varied winds and convective mixing produce a primary black hole mass function with twin peaks near 8 and 13 solar masses in most variations, the higher peak dominated by mass-ratio-reversal systems, with rates varying by a factor of six.
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Mergers via failed common envelope as a route towards intermediate-mass stripped stars
Failed common envelope mergers yield 6-14 solar mass stripped stars consistent with long-lived core He-burning objects that appear single or in wide binaries from hierarchical triples.
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Nucleosynthesis in the fast ejecta of a neutron star merger
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
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Simulations of Interacting Binary Systems -- Pathways to Radio Bright GRB Progenitors
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.