The sensitivity of presupernova neutrinos to stellar evolution models

Chinami Kato, Ryosuke Hirai, Hiroki Nagakura

Research output: Contribution to journalArticlepeer-review

Abstract

We examine the sensitivity of neutrino emissions to stellar evolution models for a 15M progenitor, paying particular attention to a phase prior to the collapse. We demonstrate that the number luminosities in both electron-type neutrinos (νe) and their anti-partners (¯ νe) differ by more than an order of magnitude by changing spatial resolutions and nuclear network sizes on stellar evolution models. We also develop a phenomenological model to capture the essential trend of the diversity, in which neutrino luminosities are expressed as a function of central density, temperature and electron fraction. In the analysis, we show that neutrino luminosity can be well characterized by these central quantities. This analysis also reveals that the most influential quantity to the time evolution of νe luminosity is matter density, while it is temperature for ν¯e. These qualitative trends will be useful and applicable to constrain the physical state of progenitors at the final stages of stellar evolution from future neutrino observations, although more detailed systematic studies including various mass progenitors are required to assess the applicability.

Original languageEnglish
JournalUnknown Journal
Publication statusPublished - 2020 May 6

Keywords

  • Neutrinos
  • Stars:evolution
  • Stars:massive
  • Supernovae:general

ASJC Scopus subject areas

  • General

Fingerprint Dive into the research topics of 'The sensitivity of presupernova neutrinos to stellar evolution models'. Together they form a unique fingerprint.

Cite this