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.
The Progenitor of the Type IIb SN 2008ax Revisited
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Hubble Space Telescope observations of the site of the supernova (SN) 2008ax obtained in 2011 and 2013 reveal that the possible progenitor object detected in pre-explosion images was in fact multiple. Four point sources are resolved in the new, higher-resolution images. We identify one of the sources with the fading SN. The other three objects are consistent with single supergiant stars. We conclude that their light contaminated the previously identified progenitor candidate. After subtraction of these stars, the progenitor appears to be significantly fainter and bluer than previously measured. Post-explosion photometry at the SN location indicates that the progenitor object has disappeared. If single, the progenitor is compatible with a supergiant star of B to mid-A spectral type, while a Wolf-Rayet (WR) star would be too luminous in the ultraviolet to account for the observations. Moreover, our hydrodynamical modelling shows the pre-explosion mass was $4-5$ $M_\odot$ and the radius was $30-50$ $R_\odot$, which is incompatible with a WR progenitor. We present a possible interacting binary progenitor computed with our evolutionary models that reproduces all the observational evidence. A companion star as luminous as an O9-B0 main-sequence star may have remained after the explosion.
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2026 2verdicts
UNVERDICTED 2representative citing papers
Late-time data on SN 2017dio yield mass-loss rates of ~0.2 M_sun/yr peak and ~0.06 typical, with H-rich CSM from a companion and dust masses 0.001-0.02 M_sun, indicating sudden mass-loss increase.
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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Late-time evolution of the interacting stripped-envelope supernova 2017dio
Late-time data on SN 2017dio yield mass-loss rates of ~0.2 M_sun/yr peak and ~0.06 typical, with H-rich CSM from a companion and dust masses 0.001-0.02 M_sun, indicating sudden mass-loss increase.