Enhanced mass-loss rate evolution of stars with ≥18 Mand missing optically observed type II core-collapse supernovae

Roni Anna Gofman, Naomi Gluck, Noam Soker

Research output: Contribution to journalArticlepeer-review

Abstract

We evolve stellar models with zero-age main-sequence (ZAMS) mass of MZAMS ≥ 18 M≥ 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 explore what level of enhanced mass-loss rate during the instability strip would be necessary to explain the 'red supergiant problem'. This problem refers to the dearth of observed core-collapse supernovae progenitors with MZAMS ≥ 18 M≥. Namely, we examine what enhanced mass-loss rate could make it possible for all these stars actually to explode as core-collapse supernovae (CCSNe). We find that the mass-loss rate should increase by a factor of at least about 10. We reach this conclusion by analysing the hydrogen mass in the stellar envelope and the optical depth of the dusty wind at the explosion, and crudely estimate that under our assumptions only about a fifth of these stars explode as unobscured SNe II and SNe IIb. About 10-15 per cent end as obscured SNe II that are infrared-bright but visibly very faint, and the rest, about 65-70 per cent, end as SNe Ibc. However, the statistical uncertainties are still too significant to decide whether many stars with MZAMS ≥ 18 M≥ 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.

Original languageEnglish
Pages (from-to)5230-5238
Number of pages9
JournalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume494
Issue number4
DOIs
StatePublished - 1 Jun 2020

Keywords

  • outflows
  • stars: Mass-loss
  • stars: Massive
  • stars: Winds
  • supernovae: General

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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