Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
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4 Pith papers cite this work. Polarity classification is still indexing.
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Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
New CCSN yield tables at varying metallicities are inserted into galactic chemical evolution models and tuned to reproduce the Si-group and Fe-group abundances measured by Hitomi in the Perseus Cluster.
New 17O+α and 22Ne+α rates increase weak s-process yields by tens of times in Z=10^{-3} stars of 15-30 solar masses.
citing papers explorer
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Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models
Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.
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Pulsational mass loss from supermassive stars creates the compact shells of Little Red Dots
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
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Revisiting the Perseus Cluster II: Metallicity-Dependence of Massive Stars and Chemical Enrichment History
New CCSN yield tables at varying metallicities are inserted into galactic chemical evolution models and tuned to reproduce the Si-group and Fe-group abundances measured by Hitomi in the Perseus Cluster.
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The impact of new ($\alpha$, n) reaction rates on the weak s-process in metal-poor massive stars
New 17O+α and 22Ne+α rates increase weak s-process yields by tens of times in Z=10^{-3} stars of 15-30 solar masses.