Ensemble characteristics of the ZZ Ceti stars
Autor(a) principal: | |
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Data de Publicação: | 2006 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108923 |
Resumo: | We present the observed pulsation spectra of all known noninteracting ZZ Ceti stars (hydrogen atmosphere white dwarf variables [DAVs]) and examine changes in their pulsation properties across the instability strip.We confirm the well-established trend of increasing pulsation period with decreasing effective temperature across the ZZ Ceti instability strip. We do not find a dramatic order-of-magnitude increase in the number of observed independent modes in ZZ Ceti stars, traversing from the hot to the cool edge of the instability strip; we find that the cool DAVs have one more mode on average than the hot DAVs. We confirm the initial increase in pulsation amplitude at the blue edge and find strong evidence of a decline in amplitude prior to the red edge.We present the first observational evidence that ZZ Ceti stars lose pulsation energy just before pulsations shut down at the empirical red edge of the instability strip. |
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Mukadam, Anjum ShaguftaMontgomery, Michael HoustonWinget, Donald EarlKepler, Souza OliveiraClemens, J. Christopher2015-01-14T02:16:00Z20060004-637Xhttp://hdl.handle.net/10183/108923000538161We present the observed pulsation spectra of all known noninteracting ZZ Ceti stars (hydrogen atmosphere white dwarf variables [DAVs]) and examine changes in their pulsation properties across the instability strip.We confirm the well-established trend of increasing pulsation period with decreasing effective temperature across the ZZ Ceti instability strip. We do not find a dramatic order-of-magnitude increase in the number of observed independent modes in ZZ Ceti stars, traversing from the hot to the cool edge of the instability strip; we find that the cool DAVs have one more mode on average than the hot DAVs. We confirm the initial increase in pulsation amplitude at the blue edge and find strong evidence of a decline in amplitude prior to the red edge.We present the first observational evidence that ZZ Ceti stars lose pulsation energy just before pulsations shut down at the empirical red edge of the instability strip.application/pdfengThe astrophysical journal. Chicago. Vol. 640, no. 2, pt. 1 (Apr. 2006), p. 956-965Estrelas variaveisPulsacoes estelaresAnãs brancasStars: oscillationsStars: variables: otherWhite dwarfsEnsemble characteristics of the ZZ Ceti starsEstrangeiroinfo: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:UFRGSORIGINAL000538161.pdf000538161.pdfTexto completo (inglês)application/pdf233532http://www.lume.ufrgs.br/bitstream/10183/108923/1/000538161.pdf23ba963082b63cd43eec683759b6cec2MD51TEXT000538161.pdf.txt000538161.pdf.txtExtracted Texttext/plain55370http://www.lume.ufrgs.br/bitstream/10183/108923/2/000538161.pdf.txt5b8834bdb321fc869f5fbb2098e9c495MD52THUMBNAIL000538161.pdf.jpg000538161.pdf.jpgGenerated Thumbnailimage/jpeg1826http://www.lume.ufrgs.br/bitstream/10183/108923/3/000538161.pdf.jpga4c95c6f145eddd7349e0ff93a8c41fcMD5310183/1089232018-10-23 08:39:44.383oai:www.lume.ufrgs.br:10183/108923Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-23T11:39:44Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Ensemble characteristics of the ZZ Ceti stars |
title |
Ensemble characteristics of the ZZ Ceti stars |
spellingShingle |
Ensemble characteristics of the ZZ Ceti stars Mukadam, Anjum Shagufta Estrelas variaveis Pulsacoes estelares Anãs brancas Stars: oscillations Stars: variables: other White dwarfs |
title_short |
Ensemble characteristics of the ZZ Ceti stars |
title_full |
Ensemble characteristics of the ZZ Ceti stars |
title_fullStr |
Ensemble characteristics of the ZZ Ceti stars |
title_full_unstemmed |
Ensemble characteristics of the ZZ Ceti stars |
title_sort |
Ensemble characteristics of the ZZ Ceti stars |
author |
Mukadam, Anjum Shagufta |
author_facet |
Mukadam, Anjum Shagufta Montgomery, Michael Houston Winget, Donald Earl Kepler, Souza Oliveira Clemens, J. Christopher |
author_role |
author |
author2 |
Montgomery, Michael Houston Winget, Donald Earl Kepler, Souza Oliveira Clemens, J. Christopher |
author2_role |
author author author author |
dc.contributor.author.fl_str_mv |
Mukadam, Anjum Shagufta Montgomery, Michael Houston Winget, Donald Earl Kepler, Souza Oliveira Clemens, J. Christopher |
dc.subject.por.fl_str_mv |
Estrelas variaveis Pulsacoes estelares Anãs brancas |
topic |
Estrelas variaveis Pulsacoes estelares Anãs brancas Stars: oscillations Stars: variables: other White dwarfs |
dc.subject.eng.fl_str_mv |
Stars: oscillations Stars: variables: other White dwarfs |
description |
We present the observed pulsation spectra of all known noninteracting ZZ Ceti stars (hydrogen atmosphere white dwarf variables [DAVs]) and examine changes in their pulsation properties across the instability strip.We confirm the well-established trend of increasing pulsation period with decreasing effective temperature across the ZZ Ceti instability strip. We do not find a dramatic order-of-magnitude increase in the number of observed independent modes in ZZ Ceti stars, traversing from the hot to the cool edge of the instability strip; we find that the cool DAVs have one more mode on average than the hot DAVs. We confirm the initial increase in pulsation amplitude at the blue edge and find strong evidence of a decline in amplitude prior to the red edge.We present the first observational evidence that ZZ Ceti stars lose pulsation energy just before pulsations shut down at the empirical red edge of the instability strip. |
publishDate |
2006 |
dc.date.issued.fl_str_mv |
2006 |
dc.date.accessioned.fl_str_mv |
2015-01-14T02:16:00Z |
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/10183/108923 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
000538161 |
identifier_str_mv |
0004-637X 000538161 |
url |
http://hdl.handle.net/10183/108923 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Chicago. Vol. 640, no. 2, pt. 1 (Apr. 2006), p. 956-965 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
application/pdf |
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