Case C mass transfer in binaries with 10-20 solar mass donors naturally produces the dense, nearby CSM required to power interacting supernovae and may account for 13 percent of core-collapse progenitors.
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3D MHD simulations of CCSN remnants from RSG and WR stars show faster shocks from photoionization and CSM expansion, plus coherent reflected shocks in WR cases, with weakly magnetized bubbles limiting PeV acceleration.
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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Interacting Binary Stars as Progenitors for Interacting Supernovae
Case C mass transfer in binaries with 10-20 solar mass donors naturally produces the dense, nearby CSM required to power interacting supernovae and may account for 13 percent of core-collapse progenitors.
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Multi-Dimensional MHD simulations of young Core-Collapse Supernova Remnants
3D MHD simulations of CCSN remnants from RSG and WR stars show faster shocks from photoionization and CSM expansion, plus coherent reflected shocks in WR cases, with weakly magnetized bubbles limiting PeV acceleration.
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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.