Properties of convective oxygen and silicon burning shells in supernova progenitors

Christine Collins, Bernhard Müller, Alexander Heger

Research output: Contribution to journalArticleResearchpeer-review

21 Citations (Scopus)

Abstract

Recent 3D simulations have suggested that convective seed perturbations from shell burning can play an important role in triggering neutrino-driven supernova explosions. Since isolated simulations cannot determine whether this perturbation-aided mechanism is of general relevance across the progenitor mass range, we here investigate the pertinent properties of convective oxygen and silicon burning shells in a broad range of pre-supernova stellar evolution models. We find that conditions for perturbation-aided explosions are most favourable in the extended oxygen shells of progenitors between about 16 and 26 solar masses, which exhibit large-scale convective overturn with high convective Mach numbers. Although the highest convective Mach numbers of up to 0.3 are reached in the oxygen shells of low-mass progenitors, convection is typically dominated by small-scale modes in these shells, which implies a more modest role of initial perturbations in the explosion mechanism. Convective silicon burning rarely provides the high Mach numbers and large-scale perturbations required for perturbation-aided explosions. We also find that about 40 per cent of progenitors between 16 and 26 solar masses exhibit simultaneous oxygen and neon burning in the same convection zone as a result of a shell merger shortly before collapse.

Original languageEnglish
Pages (from-to)1695-1704
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Volume473
Issue number2
DOIs
Publication statusPublished - 1 Jan 2018

Keywords

  • convection
  • stars: evolution
  • stars: massive
  • supernovae: general

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