University of Hertfordshire

From the same journal

From the same journal

By the same authors

Documents

  • 2006.12517v1

    Accepted author manuscript, 645 KB, PDF document

  • Mattis Magg
  • Thomas Nordlander
  • Simon C. O. Glover
  • Camilla J. Hansen
  • Miho Ishigaki
  • Alexander Heger
  • Ralf S. Klessen
  • Chiaki Kobayashi
  • Ken'ichi Nomoto
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Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
DOIs
Publication statusPublished - 29 Aug 2020

Abstract

To date no metal-free stars have been identified by direct observations. The most common method of constraining their properties is searching the spectra of the most metal-poor stars for the chemical elements created in the first stars and their supernova. In this approach, modelled supernova yields are compared to the observed abundance patterns in extremely metal-poor stars. The method typically only uses the abundance ratios, i.e., the yields are diluted to the observed level. Following the usual assumption of spherical symmetry we compute a simple lower limit of the mass a supernova can mix with and find that it is consistent with all published simulations of early chemical enrichment in the interstellar medium. For three different cases, we demonstrate that this dilution limit can change the conclusions from the abundance fitting. There is a large discrepancy between the dilution found in simulations of SN explosions in minihaloes and the dilution assumed in many abundance fits. Limiting the dilution can significantly alter the likelihood of which supernovae are possible progenitors of observed CEMP-no stars. In particular, some of the faint, very low-yield SNe, which have been suggested as models for the abundance pattern of SMSS0313-6708, cannot explain the measured metal abundances, as their predicted metal yields are too small by two orders of magnitude. Altogether, the new dilution model presented here emphasizes the need to better understand the mixing and dilution behaviour of aspherical SNe.

Notes

10 pages, 6 figures, submitted to MNRAS

ID: 22573454