Fates of the most massive primordial stars

Ke-Jung Chen, Alexander Heger, Ann Almgren, Stan Woosley

Research output: Chapter in Book/Report/Conference proceedingConference PaperResearch

Abstract

We present our results of numerical simulations of the most massive primordial stars. For the extremely massive non-rotating Pop III stars over 300M, they would simply die as black holes. But the Pop III stars with initial masses 140 - 260M may have died as gigantic explosions called pair-instability supernovae (PSNe). We use a new radiation-hydrodynamics code CASTRO to study evolution of PSNe. Our models follow the entire explosive burning and the explosion until the shock breaks out from the stellar surface. In our simulations, we find that fluid instabilities occurred during the explosion. These instabilities are driven by both nuclear burning and hydrodynamical instability. In the red supergiant models, fluid instabilities can lead to significant mixing of supernova ejecta and alter the observational signature.

Original languageEnglish
Title of host publicationFirst Stars IV - From Hayashi to the Future
Subtitle of host publicationKyoto, Japan; 21-25 May 2012
EditorsMasayuki Umemura, Kazuyuki Omukai
Place of PublicationUSA
PublisherAIP Publishing
Pages340-342
Number of pages3
ISBN (Print)9780735410923
DOIs
Publication statusPublished - 2012
EventConference on FIRST STARS - From Hayashi to the Future 2012 - Kyoto, Japan
Duration: 21 May 201225 May 2012
Conference number: 4th

Publication series

NameAIP Conference Proceedings
PublisherAIP Publishing
Volume1480
ISSN (Print)0094-243x

Conference

ConferenceConference on FIRST STARS - From Hayashi to the Future 2012
CountryJapan
CityKyoto
Period21/05/1225/05/12

Keywords

  • Pair-Instability Supernovae
  • Pop III Stars

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