English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Theoretical models suggest that the first stars in the universe could havebeen very massive, with typical masses $\gtrsim$ 100 \Msun. Many of them mighthave died as energetic thermonuclear explosions known as pair-instabilitysupernovae (PSNe). We present multidimensional numerical simulations of PSNewith the new radiation-hydrodynamics code CASTRO. Our models capture allexplosive burning and follow the explosion until the shock breaks out from thestellar surface. We find that fluid instabilities driven by oxygen and heliumburning arise at the upper and lower boundaries of the oxygen shell $\sim$ 20 -100 sec after the explosion begins. Later, when the shock reaches the hydrogenenvelope a strong reverse shock forms that rapidly develops additionalRayleigh-Taylor instabilities. In red supergiant progenitors, the amplitudes ofthese instabilities are sufficient to mix the supernova's ejecta and alter itsobservational signature. Our results provide useful predictions for thedetection of PSNe by forthcoming telescopes.

Multidimensional Simulations of Thermonuclear Supernovae from the First Stars