Type Ic core-collapse supernovae explode in systematically younger environments than Types II, IIb, and Ib, indicating they arise from more massive progenitors via a distinct channel.
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4 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.
Observations show a slight rise in stripped-envelope supernovae relative to hydrogen-rich ones at higher metallicities, with binary-interaction or rotation models able to match the trends though no unique scenario fits best.
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.
citing papers explorer
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A statistical study of the environmental age of core-collapse supernovae based on VLT/MUSE integral-field-unit spectroscopy
Type Ic core-collapse supernovae explode in systematically younger environments than Types II, IIb, and Ib, indicating they arise from more massive progenitors via a distinct channel.
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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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Relative frequencies of core-collapse supernovae as a function of metallicity: observations vs theoretical predictions
Observations show a slight rise in stripped-envelope supernovae relative to hydrogen-rich ones at higher metallicities, with binary-interaction or rotation models able to match the trends though no unique scenario fits best.
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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.