Comparison of statistical treatments for the equation of state for core-collapse supernovae
Autor(a) principal: | |
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Data de Publicação: | 2009 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108969 |
Resumo: | Neutrinos emitted during the collapse, bounce, and subsequent explosion provide information about supernova dynamics. The neutrino spectra are determined by weak interactions with nuclei and nucleons in the inner regions of the star, and thus the neutrino spectra are determined by the composition of matter. The composition of stellar matter at temperature ranging from T = 1–3 MeV and densities ranging from 10−5 to 0.1 times the saturation density is explored. We examine the single-nucleus approximation commonly used in describing dense matter in supernova simulations and show that while the approximation is accurate for predicting the energy and pressure at most densities, the predicted compositions are less accurate, varying by 50% or more at the largest densities. We find that as the temperature and density increase, the single nucleus approximation systematically overpredicts the mass number of nuclei that are actually present and underestimates the contribution from lighter nuclei which are present in significant amounts. |
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Souza, Sergio Ricardo de AzevedoSteiner, Andrew W.Lynch, William G.Donangelo, Raul JoséFamiano, Michael A.2015-01-15T02:15:08Z20090004-637Xhttp://hdl.handle.net/10183/108969000729823Neutrinos emitted during the collapse, bounce, and subsequent explosion provide information about supernova dynamics. The neutrino spectra are determined by weak interactions with nuclei and nucleons in the inner regions of the star, and thus the neutrino spectra are determined by the composition of matter. The composition of stellar matter at temperature ranging from T = 1–3 MeV and densities ranging from 10−5 to 0.1 times the saturation density is explored. We examine the single-nucleus approximation commonly used in describing dense matter in supernova simulations and show that while the approximation is accurate for predicting the energy and pressure at most densities, the predicted compositions are less accurate, varying by 50% or more at the largest densities. We find that as the temperature and density increase, the single nucleus approximation systematically overpredicts the mass number of nuclei that are actually present and underestimates the contribution from lighter nuclei which are present in significant amounts.application/pdfengThe astrophysical journal. Bristol. Vol. 707, no. 2 (Dec. 2009), p. 1495-1505Análise estatísticaComposicao estelarNeutrinosSupernovaDense matterEquation of stateSupernovae: generalComparison of statistical treatments for the equation of state for core-collapse supernovaeEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL000729823.pdf000729823.pdfTexto completo (inglês)application/pdf822388http://www.lume.ufrgs.br/bitstream/10183/108969/1/000729823.pdf3c20c414d534389e428facba609a2c73MD51TEXT000729823.pdf.txt000729823.pdf.txtExtracted Texttext/plain59173http://www.lume.ufrgs.br/bitstream/10183/108969/2/000729823.pdf.txt029b414f9aed2e98eb83da17559746d3MD52THUMBNAIL000729823.pdf.jpg000729823.pdf.jpgGenerated Thumbnailimage/jpeg2241http://www.lume.ufrgs.br/bitstream/10183/108969/3/000729823.pdf.jpgcf3b4eed8e201a2947b874182c038a8bMD5310183/1089692018-10-23 08:39:47.39oai:www.lume.ufrgs.br:10183/108969Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-23T11:39:47Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
title |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
spellingShingle |
Comparison of statistical treatments for the equation of state for core-collapse supernovae Souza, Sergio Ricardo de Azevedo Análise estatística Composicao estelar Neutrinos Supernova Dense matter Equation of state Supernovae: general |
title_short |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
title_full |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
title_fullStr |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
title_full_unstemmed |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
title_sort |
Comparison of statistical treatments for the equation of state for core-collapse supernovae |
author |
Souza, Sergio Ricardo de Azevedo |
author_facet |
Souza, Sergio Ricardo de Azevedo Steiner, Andrew W. Lynch, William G. Donangelo, Raul José Famiano, Michael A. |
author_role |
author |
author2 |
Steiner, Andrew W. Lynch, William G. Donangelo, Raul José Famiano, Michael A. |
author2_role |
author author author author |
dc.contributor.author.fl_str_mv |
Souza, Sergio Ricardo de Azevedo Steiner, Andrew W. Lynch, William G. Donangelo, Raul José Famiano, Michael A. |
dc.subject.por.fl_str_mv |
Análise estatística Composicao estelar Neutrinos Supernova |
topic |
Análise estatística Composicao estelar Neutrinos Supernova Dense matter Equation of state Supernovae: general |
dc.subject.eng.fl_str_mv |
Dense matter Equation of state Supernovae: general |
description |
Neutrinos emitted during the collapse, bounce, and subsequent explosion provide information about supernova dynamics. The neutrino spectra are determined by weak interactions with nuclei and nucleons in the inner regions of the star, and thus the neutrino spectra are determined by the composition of matter. The composition of stellar matter at temperature ranging from T = 1–3 MeV and densities ranging from 10−5 to 0.1 times the saturation density is explored. We examine the single-nucleus approximation commonly used in describing dense matter in supernova simulations and show that while the approximation is accurate for predicting the energy and pressure at most densities, the predicted compositions are less accurate, varying by 50% or more at the largest densities. We find that as the temperature and density increase, the single nucleus approximation systematically overpredicts the mass number of nuclei that are actually present and underestimates the contribution from lighter nuclei which are present in significant amounts. |
publishDate |
2009 |
dc.date.issued.fl_str_mv |
2009 |
dc.date.accessioned.fl_str_mv |
2015-01-15T02:15:08Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/108969 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
000729823 |
identifier_str_mv |
0004-637X 000729823 |
url |
http://hdl.handle.net/10183/108969 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Bristol. Vol. 707, no. 2 (Dec. 2009), p. 1495-1505 |
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info:eu-repo/semantics/openAccess |
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openAccess |
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application/pdf |
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