Si, O, Ne, and C shell burning

Casey Meakin, W David Arnett

Research output: Contribution to journalArticle

Abstract

We simulate the reactive-hydrodynamic flow for a variety of convective shell burning epochs in supernova progenitor models. The neutrino-cooled stages of carbon, neon, oxygen, and silicon burning are simulated in two and three dimensions. Even in the absence of rotation significant symmetry breaking occurs (10% in rms variation in thermodynamic variables such as temperature and density). These distortions are caused by turbulent convection interacting with stably stratified boundaries. Strong interactions of multiple active shells is seen; it is mediated by waves generated by convection. Some implications for supernova progenitors are presented.

Original languageEnglish (US)
Pages (from-to)296-297
Number of pages2
JournalProceedings of the International Astronomical Union
Volume2
Issue numberS239
DOIs
StatePublished - Aug 2006

Fingerprint

supernovae
convection
shell
Neon
neon
silicon
symmetry
broken symmetry
Hydrodynamics
neutrinos
thermodynamics
hydrodynamics
time measurement
Thermodynamics
Silicon
oxygen
Carbon
Oxygen
carbon
temperature

Keywords

  • Convection
  • Methods: numerical
  • Neutrinos
  • Nucleosynthesis
  • Stars: evolution
  • Stars: supernovae
  • Turbulence
  • Waves

ASJC Scopus subject areas

  • Physics and Astronomy (miscellaneous)
  • Aerospace Engineering

Cite this

Si, O, Ne, and C shell burning. / Meakin, Casey; Arnett, W David.

In: Proceedings of the International Astronomical Union, Vol. 2, No. S239, 08.2006, p. 296-297.

Research output: Contribution to journalArticle

@article{9e641fefdf4a472a9c6059733e6f5c19,
title = "Si, O, Ne, and C shell burning",
abstract = "We simulate the reactive-hydrodynamic flow for a variety of convective shell burning epochs in supernova progenitor models. The neutrino-cooled stages of carbon, neon, oxygen, and silicon burning are simulated in two and three dimensions. Even in the absence of rotation significant symmetry breaking occurs (10{\%} in rms variation in thermodynamic variables such as temperature and density). These distortions are caused by turbulent convection interacting with stably stratified boundaries. Strong interactions of multiple active shells is seen; it is mediated by waves generated by convection. Some implications for supernova progenitors are presented.",
keywords = "Convection, Methods: numerical, Neutrinos, Nucleosynthesis, Stars: evolution, Stars: supernovae, Turbulence, Waves",
author = "Casey Meakin and Arnett, {W David}",
year = "2006",
month = "8",
doi = "10.1017/S1743921307000580",
language = "English (US)",
volume = "2",
pages = "296--297",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",
number = "S239",

}

TY - JOUR

T1 - Si, O, Ne, and C shell burning

AU - Meakin, Casey

AU - Arnett, W David

PY - 2006/8

Y1 - 2006/8

N2 - We simulate the reactive-hydrodynamic flow for a variety of convective shell burning epochs in supernova progenitor models. The neutrino-cooled stages of carbon, neon, oxygen, and silicon burning are simulated in two and three dimensions. Even in the absence of rotation significant symmetry breaking occurs (10% in rms variation in thermodynamic variables such as temperature and density). These distortions are caused by turbulent convection interacting with stably stratified boundaries. Strong interactions of multiple active shells is seen; it is mediated by waves generated by convection. Some implications for supernova progenitors are presented.

AB - We simulate the reactive-hydrodynamic flow for a variety of convective shell burning epochs in supernova progenitor models. The neutrino-cooled stages of carbon, neon, oxygen, and silicon burning are simulated in two and three dimensions. Even in the absence of rotation significant symmetry breaking occurs (10% in rms variation in thermodynamic variables such as temperature and density). These distortions are caused by turbulent convection interacting with stably stratified boundaries. Strong interactions of multiple active shells is seen; it is mediated by waves generated by convection. Some implications for supernova progenitors are presented.

KW - Convection

KW - Methods: numerical

KW - Neutrinos

KW - Nucleosynthesis

KW - Stars: evolution

KW - Stars: supernovae

KW - Turbulence

KW - Waves

UR - http://www.scopus.com/inward/record.url?scp=36949034118&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=36949034118&partnerID=8YFLogxK

U2 - 10.1017/S1743921307000580

DO - 10.1017/S1743921307000580

M3 - Article

AN - SCOPUS:36949034118

VL - 2

SP - 296

EP - 297

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

IS - S239

ER -