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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A triple-star channel with two common envelope evolution phases produces merging black hole binaries with positive average χ_eff and a tail of negative values.
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.
Late-time IR spectroscopy of SN 2024ggi shows varied line morphologies implying chemical inhomogeneity and aspherical ionization, with modeling favoring 12-15 solar mass progenitors but only high-mass energetic 3D simulations matching the observed Ni mixing extent.
Depositing stellar luminosity in an inner shell and cooling low-density outer cells produces a stable pulsating 3D red supergiant model for common envelope simulations without relaxation.
No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.
N6946-BH1's remnant is roughly 10 times fainter than its progenitor while stellar merger remnants are 10-100 times brighter, and asymmetric dust cannot explain the difference.
High-metallicity star cluster simulations produce black hole mergers with masses and ratios consistent with recent LVK detections, unlike low-metallicity models.
Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.
Hydrodynamic simulations of three pairs of jittering jets in a CCSN reproduce the ring-and-bar morphology of SNR G11.2-0.3.
SN 2024abfl is a sub-luminous Type IIP event from a compact progenitor exploding with energy at most 0.05 foe and nickel mass 0.003 solar masses.
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Red vs. Blue: How metallicity shapes black hole dynamics and mergers in dense star clusters
High-metallicity star cluster simulations produce black hole mergers with masses and ratios consistent with recent LVK detections, unlike low-metallicity models.