Redefining the empirical ZZ Ceti instability strip
Autor(a) principal: | |
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Data de Publicação: | 2004 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108915 |
Resumo: | We use the new ZZ Ceti stars (hydrogen-atmosphere white dwarf variables; DAVs) discovered within the Sloan Digital Sky Survey (Mukadam et al. 2004) to redefine the empirical ZZ Ceti instability strip. This is the first time since the discovery of white dwarf variables in 1968 that we have a homogeneous set of spectra acquired using the same instrument on the same telescope, and with consistent data reductions, for a statistically significant sample of ZZ Ceti stars. The homogeneity of the spectra reduces the scatter in the spectroscopic temperatures, and we find a narrow instability strip of width ~950 K, from 10,850 to 11,800 K. We question the purity of the DAV instability strip, as we find several nonvariables within. We present our best fit for the red edge and our constraint for the blue edge of the instability strip, determined using a statistical approach. |
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Mukadam, Anjum ShaguftaWinget, Donald EarlVon Hippel, Theodore A.Montgomery, Michael HoustonKepler, Souza OliveiraCosta, Alex Fabiano Murillo da2015-01-14T02:15:56Z20040004-637Xhttp://hdl.handle.net/10183/108915000504032We use the new ZZ Ceti stars (hydrogen-atmosphere white dwarf variables; DAVs) discovered within the Sloan Digital Sky Survey (Mukadam et al. 2004) to redefine the empirical ZZ Ceti instability strip. This is the first time since the discovery of white dwarf variables in 1968 that we have a homogeneous set of spectra acquired using the same instrument on the same telescope, and with consistent data reductions, for a statistically significant sample of ZZ Ceti stars. The homogeneity of the spectra reduces the scatter in the spectroscopic temperatures, and we find a narrow instability strip of width ~950 K, from 10,850 to 11,800 K. We question the purity of the DAV instability strip, as we find several nonvariables within. We present our best fit for the red edge and our constraint for the blue edge of the instability strip, determined using a statistical approach.application/pdfengThe Astrophysical journal. Chicago. Vol. 612, no. 2 pt. 1 (Sept. 2004), p. 1052-1059HidrogênioAtmosferas estelaresPulsacoes estelaresEspectros estelaresEstrelas variaveisAnãs brancasStars: oscillationsStars: variables: otherWhite dwarfsRedefining the empirical ZZ Ceti instability stripEstrangeiroinfo: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:UFRGSORIGINAL000504032.pdf000504032.pdfTexto completo (inglês)application/pdf200354http://www.lume.ufrgs.br/bitstream/10183/108915/1/000504032.pdf32fc74747c26b1edca1484aa83f2115aMD51TEXT000504032.pdf.txt000504032.pdf.txtExtracted Texttext/plain38420http://www.lume.ufrgs.br/bitstream/10183/108915/2/000504032.pdf.txt20e21b36eb9dbae3182f5abe78524301MD52THUMBNAIL000504032.pdf.jpg000504032.pdf.jpgGenerated Thumbnailimage/jpeg1860http://www.lume.ufrgs.br/bitstream/10183/108915/3/000504032.pdf.jpgdbad42df0436454e87423a5935167a30MD5310183/1089152018-10-23 08:39:54.932oai:www.lume.ufrgs.br:10183/108915Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-23T11:39:54Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Redefining the empirical ZZ Ceti instability strip |
title |
Redefining the empirical ZZ Ceti instability strip |
spellingShingle |
Redefining the empirical ZZ Ceti instability strip Mukadam, Anjum Shagufta Hidrogênio Atmosferas estelares Pulsacoes estelares Espectros estelares Estrelas variaveis Anãs brancas Stars: oscillations Stars: variables: other White dwarfs |
title_short |
Redefining the empirical ZZ Ceti instability strip |
title_full |
Redefining the empirical ZZ Ceti instability strip |
title_fullStr |
Redefining the empirical ZZ Ceti instability strip |
title_full_unstemmed |
Redefining the empirical ZZ Ceti instability strip |
title_sort |
Redefining the empirical ZZ Ceti instability strip |
author |
Mukadam, Anjum Shagufta |
author_facet |
Mukadam, Anjum Shagufta Winget, Donald Earl Von Hippel, Theodore A. Montgomery, Michael Houston Kepler, Souza Oliveira Costa, Alex Fabiano Murillo da |
author_role |
author |
author2 |
Winget, Donald Earl Von Hippel, Theodore A. Montgomery, Michael Houston Kepler, Souza Oliveira Costa, Alex Fabiano Murillo da |
author2_role |
author author author author author |
dc.contributor.author.fl_str_mv |
Mukadam, Anjum Shagufta Winget, Donald Earl Von Hippel, Theodore A. Montgomery, Michael Houston Kepler, Souza Oliveira Costa, Alex Fabiano Murillo da |
dc.subject.por.fl_str_mv |
Hidrogênio Atmosferas estelares Pulsacoes estelares Espectros estelares Estrelas variaveis Anãs brancas |
topic |
Hidrogênio Atmosferas estelares Pulsacoes estelares Espectros estelares Estrelas variaveis Anãs brancas Stars: oscillations Stars: variables: other White dwarfs |
dc.subject.eng.fl_str_mv |
Stars: oscillations Stars: variables: other White dwarfs |
description |
We use the new ZZ Ceti stars (hydrogen-atmosphere white dwarf variables; DAVs) discovered within the Sloan Digital Sky Survey (Mukadam et al. 2004) to redefine the empirical ZZ Ceti instability strip. This is the first time since the discovery of white dwarf variables in 1968 that we have a homogeneous set of spectra acquired using the same instrument on the same telescope, and with consistent data reductions, for a statistically significant sample of ZZ Ceti stars. The homogeneity of the spectra reduces the scatter in the spectroscopic temperatures, and we find a narrow instability strip of width ~950 K, from 10,850 to 11,800 K. We question the purity of the DAV instability strip, as we find several nonvariables within. We present our best fit for the red edge and our constraint for the blue edge of the instability strip, determined using a statistical approach. |
publishDate |
2004 |
dc.date.issued.fl_str_mv |
2004 |
dc.date.accessioned.fl_str_mv |
2015-01-14T02:15:56Z |
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/10183/108915 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
000504032 |
identifier_str_mv |
0004-637X 000504032 |
url |
http://hdl.handle.net/10183/108915 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The Astrophysical journal. Chicago. Vol. 612, no. 2 pt. 1 (Sept. 2004), p. 1052-1059 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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application/pdf |
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