Weak decay processes in pre-supernova core evolution within the gross theory

The beta decay and electron capture rates are of fundamental importance in the evolution of massive stars in a pre-supernova core. The beta decay process gives its contribution by emitting electrons in the plasma of the stellar core, thereby increasing pressure, which in turn increases the temperatu...

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Detalles Bibliográficos
Autores principales: Ferreira, R. C., Dimarco, A. J., Samana, Arturo Rodolfo, Barbero, César Alberto
Formato: Articulo
Lenguaje:Inglés
Publicado: 2014
Materias:
Ciencias Exactas
atomic processes
nuclear reactions, nucleosynthesis, abundances
supernovae: general
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/85122
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-85122
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Exactas
atomic processes
nuclear reactions, nucleosynthesis, abundances
supernovae: general
spellingShingle Ciencias Exactas
atomic processes
nuclear reactions, nucleosynthesis, abundances
supernovae: general
Ferreira, R. C.
Dimarco, A. J.
Samana, Arturo Rodolfo
Barbero, César Alberto
Weak decay processes in pre-supernova core evolution within the gross theory
topic_facet Ciencias Exactas
atomic processes
nuclear reactions, nucleosynthesis, abundances
supernovae: general
description The beta decay and electron capture rates are of fundamental importance in the evolution of massive stars in a pre-supernova core. The beta decay process gives its contribution by emitting electrons in the plasma of the stellar core, thereby increasing pressure, which in turn increases the temperature. From the other side, the electron capture removes free electrons from the plasma of the star core contributing to the reduction of pressure and temperature. In this work we calculate the beta decay and electron capture rates in stellar conditions for 63 nuclei of relevance in the pre-supernova stage, employing Gross Theory as the nuclear model. We use the abundances calculated with the Saha equations in the hypothesis of nuclear statistical equilibrium to evaluate the time derivative of the fraction of electrons. Our results are compared with other evaluations available in the literature. They have shown to be one order less or equal than the calculated within other models. Our results indicate that these differences may influence the evolution of the star in the later stages of pre-supernova.
format Articulo
Articulo
author Ferreira, R. C.
Dimarco, A. J.
Samana, Arturo Rodolfo
Barbero, César Alberto
author_facet Ferreira, R. C.
Dimarco, A. J.
Samana, Arturo Rodolfo
Barbero, César Alberto
author_sort Ferreira, R. C.
title Weak decay processes in pre-supernova core evolution within the gross theory
title_short Weak decay processes in pre-supernova core evolution within the gross theory
title_full Weak decay processes in pre-supernova core evolution within the gross theory
title_fullStr Weak decay processes in pre-supernova core evolution within the gross theory
title_full_unstemmed Weak decay processes in pre-supernova core evolution within the gross theory
title_sort weak decay processes in pre-supernova core evolution within the gross theory
publishDate 2014
url http://sedici.unlp.edu.ar/handle/10915/85122
work_keys_str_mv AT ferreirarc weakdecayprocessesinpresupernovacoreevolutionwithinthegrosstheory
AT dimarcoaj weakdecayprocessesinpresupernovacoreevolutionwithinthegrosstheory
AT samanaarturorodolfo weakdecayprocessesinpresupernovacoreevolutionwithinthegrosstheory
AT barberocesaralberto weakdecayprocessesinpresupernovacoreevolutionwithinthegrosstheory
bdutipo_str Repositorios
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