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SUMMARY:Exploding Wolf-Rayet Stars - Avishai Gilkis\, Tel Aviv University
DTSTART:20230621T121500Z
DTEND:20230621T124000Z
UID:TALK202606@talks.cam.ac.uk
CONTACT:Hannah Uebler
DESCRIPTION:Wolf-Rayet (WR) stars are an advanced evolutionary stage of so
 me massive stars\, with very hot temperatures and high wind mass-loss rate
 s inferred from their spectra. Observed WR stars are thought to have cores
  too massive to explode\, and therefore collapse to black holes with no su
 pernova at the end of their evolution. Yet\, some hydrogen-poor supernovae
  exhibit spectral signatures indicating the progenitor star had a wind rem
 iniscent of WR stars. I propose that most of the exploding WR stars are no
 t those that are observed\, but rather less massive helium stars whose hyd
 rogen envelope was stripped by binary interaction. The wind mass-loss rate
  of these stripped stars becomes high only in their final evolutionary sta
 ges\, after core helium burning has ended. Using detailed binary stellar e
 volution simulations\, I show that the evolution of stripped stars can end
  in a short-lived WR phase of only a few millennia\, in contrast to hundre
 ds of millennia of their more massive WR siblings. Such lightweight WR sta
 rs can account for observed properties of type Ib/c supernovae. Employing 
 a population synthesis approach\, accounting for the formation likelihood 
 and lifetimes\, I show that the majority of exploding WR stars are the min
 ority of living WR stars.
LOCATION:The Hoyle Lecture Theatre + Zoom 
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