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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7 Pith papers cite this work. Polarity classification is still indexing.
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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.
Population synthesis of helium star-NS systems yields DNS delay time distributions that peak between 80-250 Myr across metallicities, with 15% merging within 80 Myr and over 20% after 1 Gyr.
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
Eruptive mass loss in red supergiants increases linearly with metallicity, calibrated via by-eye fits to Local Group luminosity functions, preventing initial masses above about 20 solar masses from reaching the red supergiant phase.
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.
Rotation produces only modest changes to blue loop luminosity and extent in MESA Cepheid models and cannot fix the mass discrepancy without substantial main-sequence overshooting.
citing papers explorer
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Interacting Binary Stars as Progenitors for Interacting Supernovae
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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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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Double Neutron Star Delay Times Across Cosmic Metallicities: The Role of Helium Star Progenitors
Population synthesis of helium star-NS systems yields DNS delay time distributions that peak between 80-250 Myr across metallicities, with 15% merging within 80 Myr and over 20% after 1 Gyr.
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Adiabatic Mass Loss In Binary Stars. VI. Massive Helium Binary Stars
Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.
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Calibrating Eruptive Mass Loss in Red Supergiants with Local Group Data
Eruptive mass loss in red supergiants increases linearly with metallicity, calibrated via by-eye fits to Local Group luminosity functions, preventing initial masses above about 20 solar masses from reaching the red supergiant phase.
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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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Toward a Comprehensive Grid of Cepheid Models with MESA. IV. Modest Effects of Rotation on Blue Loops
Rotation produces only modest changes to blue loop luminosity and extent in MESA Cepheid models and cannot fix the mass discrepancy without substantial main-sequence overshooting.