Chaos and turbulent nucleosynthesis prior to a supernova explosion

W David Arnett, C. Meakin, M. Viallet

Research output: Contribution to journalArticle

16 Citations (Scopus)

Abstract

Three-dimensional (3D), time dependent numerical simulations of flow of matter in stars, now have sufficient resolution to be fully turbulent. The late stages of the evolution of massive stars, leading up to core collapse to a neutron star (or black hole), and often to supernova explosion and nucleosynthesis, are strongly convective because of vigorous neutrino cooling and nuclear heating. Unlike models based on current stellar evolutionary practice, these simulations show a chaotic dynamics characteristic of highly turbulent flow. Theoretical analysis of this flow, both in the Reynolds-averaged Navier-Stokes (RANS) framework and by simple dynamic models, show an encouraging consistency with the numerical results. It may now be possible to develop physically realistic and robust procedures for convection and mixing which (unlike 3D numerical simulation) may be applied throughout the long life times of stars. In addition, a new picture of the presupernova stages is emerging which is more dynamic and interesting (i.e., predictive of new and newly observed phenomena) than our previous one.

Original languageEnglish (US)
Article number041010
JournalAIP Advances
Volume4
Issue number4
DOIs
StatePublished - 2014

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nuclear fusion
supernovae
explosions
chaos
stars
simulation
massive stars
dynamic models
turbulent flow
dynamic characteristics
neutron stars
emerging
convection
neutrinos
cooling
life (durability)
heating

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Chaos and turbulent nucleosynthesis prior to a supernova explosion. / Arnett, W David; Meakin, C.; Viallet, M.

In: AIP Advances, Vol. 4, No. 4, 041010, 2014.

Research output: Contribution to journalArticle

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