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 language | English |
---|---|
Title of host publication | First Stars IV - From Hayashi to the Future |
Subtitle of host publication | Kyoto, Japan; 21-25 May 2012 |
Editors | Masayuki Umemura, Kazuyuki Omukai |
Place of Publication | USA |
Publisher | American Institute of Physics |
Pages | 340-342 |
Number of pages | 3 |
ISBN (Print) | 9780735410923 |
DOIs | |
Publication status | Published - 2012 |
Event | Conference on FIRST STARS - From Hayashi to the Future 2012 - Kyoto, Japan Duration: 21 May 2012 → 25 May 2012 Conference number: 4th |
Publication series
Name | AIP Conference Proceedings |
---|---|
Publisher | AIP Publishing |
Volume | 1480 |
ISSN (Print) | 0094-243x |
Conference
Conference | Conference on FIRST STARS - From Hayashi to the Future 2012 |
---|---|
Country/Territory | Japan |
City | Kyoto |
Period | 21/05/12 → 25/05/12 |
Keywords
- Pair-Instability Supernovae
- Pop III Stars