http://arxiv.org/abs/1910.08021
We evolve stellar models with zero age main sequence (ZAMS) mass of $M_{\rm ZAMS} \gtrsim 18 M_\odot$ under the assumption that they experience an enhanced mass-loss rate when crossing the instability strip at high luminosities, and conclude that most of them end as type Ibc supernovae (SNe Ibc) or dust-obscured SNe II. We examine the hydrogen mass in the stellar envelope and the optical depth of the dusty wind at explosion, and crudely estimate that only about a fifth of these stars explode as unobscured SNe II and SNe IIb. About 10-15 percent end as obscured SNe II that are infrared-bright but visibly very faint, and the rest, about 65-70 percent end as SNe Ibc. Our findings have implications to the `red supergiant problem’, referring to the death of observed core-collapse supernovae with $M_{\rm ZAMS} \gtrsim 18 M_\odot$, as we conclude that it is possible that all these stars actually do explode as CCSNe. However, the statistical uncertainties are still too large to decide whether many stars with $M_{\rm ZAMS} \gtrsim 18M_\odot$ do not explode as expected in the neutrino driven explosion mechanism, or whether all of them explode as CCSNe, as expected by the jittering jets explosion mechanism.
R. Gofman, N. Gluck and N. Soker
Fri, 18 Oct 19
47/77
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