MESA binary models demonstrate that Case C Roche-lobe overflow in 10-20 Msun donors with 1000-2700 Rsun separations produces CSM matching interacting SNe and accounts for ~13% of CCSN 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.
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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.