A population-synthesis framework shows rotation and unresolved companions bias isochrone ages by a factor of at least 2 near the ZAMS and by 31% for older A stars, adding ~0.1 solar mass and ~180 Myr random uncertainties.
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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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Quantifying isochrone-based age uncertainties for rapidly rotating A-type stars
A population-synthesis framework shows rotation and unresolved companions bias isochrone ages by a factor of at least 2 near the ZAMS and by 31% for older A stars, adding ~0.1 solar mass and ~180 Myr random uncertainties.
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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.