Mode identification of pulsating white dwarfs using the Hubble Space Telescope
Autor(a) principal: | |
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Data de Publicação: | 2000 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108888 |
Resumo: | We have obtained time-resolved ultraviolet spectroscopy for the pulsating DAV stars G226-29 and G185-32 and for the pulsating DBV star PG 1351+489 with the Hubble Space Telescope Faint Object Spectrograph to compare the ultraviolet to the optical pulsation amplitude and determine the pulsation indices. We find that for essentially all observed pulsation modes, the amplitude rises to the ultraviolet as the theoretical models predict for l=1 nonradial g-modes. We do not find any pulsation mode visible only in the ultraviolet, nor any modes whose phase flips by 180° in the ultraviolet, as would be expected if high l pulsations were excited. We find one periodicity in the light curve of G185-32, at 141 s, which does not Ðt theoretical models for the change of amplitude with wavelength of g-mode pulsations. |
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Kepler, Souza OliveiraRobinson, E.L.Koester, DetlevClemens, J. ChristopherNather, R. EdwardJiang, Xiaojun2015-01-13T02:14:42Z20000004-637Xhttp://hdl.handle.net/10183/108888000274928We have obtained time-resolved ultraviolet spectroscopy for the pulsating DAV stars G226-29 and G185-32 and for the pulsating DBV star PG 1351+489 with the Hubble Space Telescope Faint Object Spectrograph to compare the ultraviolet to the optical pulsation amplitude and determine the pulsation indices. We find that for essentially all observed pulsation modes, the amplitude rises to the ultraviolet as the theoretical models predict for l=1 nonradial g-modes. We do not find any pulsation mode visible only in the ultraviolet, nor any modes whose phase flips by 180° in the ultraviolet, as would be expected if high l pulsations were excited. We find one periodicity in the light curve of G185-32, at 141 s, which does not Ðt theoretical models for the change of amplitude with wavelength of g-mode pulsations.application/pdfengThe Astrophysical journal. Chicago. Vol. 539, no. 1, pt. 1 (Aug. 2000), p. 379-391Pulsacoes estelaresFontes ultravioletas (astronômicas)Estrelas variaveisAnãs brancasStars : individual (G226-29, G185-32, PG 1351+489)Stars : oscillationsStars : variables : otherUltraviolet : starsWhite dwarfsMode identification of pulsating white dwarfs using the Hubble Space TelescopeEstrangeiroinfo: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:UFRGSORIGINAL000274928.pdf000274928.pdfTexto completo (inglês)application/pdf734045http://www.lume.ufrgs.br/bitstream/10183/108888/1/000274928.pdfcf3b36d367fc7666586bc0e3d8542e5fMD51TEXT000274928.pdf.txt000274928.pdf.txtExtracted Texttext/plain47544http://www.lume.ufrgs.br/bitstream/10183/108888/2/000274928.pdf.txt64eb1021bb1cbb40e50ee3ad908b970cMD52THUMBNAIL000274928.pdf.jpg000274928.pdf.jpgGenerated Thumbnailimage/jpeg2127http://www.lume.ufrgs.br/bitstream/10183/108888/3/000274928.pdf.jpgd2592ab3549003534ec8c7d34e27918eMD5310183/1088882018-10-23 08:37:33.309oai:www.lume.ufrgs.br:10183/108888Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-23T11:37:33Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
title |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
spellingShingle |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope Kepler, Souza Oliveira Pulsacoes estelares Fontes ultravioletas (astronômicas) Estrelas variaveis Anãs brancas Stars : individual (G226-29, G185-32, PG 1351+489) Stars : oscillations Stars : variables : other Ultraviolet : stars White dwarfs |
title_short |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
title_full |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
title_fullStr |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
title_full_unstemmed |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
title_sort |
Mode identification of pulsating white dwarfs using the Hubble Space Telescope |
author |
Kepler, Souza Oliveira |
author_facet |
Kepler, Souza Oliveira Robinson, E.L. Koester, Detlev Clemens, J. Christopher Nather, R. Edward Jiang, Xiaojun |
author_role |
author |
author2 |
Robinson, E.L. Koester, Detlev Clemens, J. Christopher Nather, R. Edward Jiang, Xiaojun |
author2_role |
author author author author author |
dc.contributor.author.fl_str_mv |
Kepler, Souza Oliveira Robinson, E.L. Koester, Detlev Clemens, J. Christopher Nather, R. Edward Jiang, Xiaojun |
dc.subject.por.fl_str_mv |
Pulsacoes estelares Fontes ultravioletas (astronômicas) Estrelas variaveis Anãs brancas |
topic |
Pulsacoes estelares Fontes ultravioletas (astronômicas) Estrelas variaveis Anãs brancas Stars : individual (G226-29, G185-32, PG 1351+489) Stars : oscillations Stars : variables : other Ultraviolet : stars White dwarfs |
dc.subject.eng.fl_str_mv |
Stars : individual (G226-29, G185-32, PG 1351+489) Stars : oscillations Stars : variables : other Ultraviolet : stars White dwarfs |
description |
We have obtained time-resolved ultraviolet spectroscopy for the pulsating DAV stars G226-29 and G185-32 and for the pulsating DBV star PG 1351+489 with the Hubble Space Telescope Faint Object Spectrograph to compare the ultraviolet to the optical pulsation amplitude and determine the pulsation indices. We find that for essentially all observed pulsation modes, the amplitude rises to the ultraviolet as the theoretical models predict for l=1 nonradial g-modes. We do not find any pulsation mode visible only in the ultraviolet, nor any modes whose phase flips by 180° in the ultraviolet, as would be expected if high l pulsations were excited. We find one periodicity in the light curve of G185-32, at 141 s, which does not Ðt theoretical models for the change of amplitude with wavelength of g-mode pulsations. |
publishDate |
2000 |
dc.date.issued.fl_str_mv |
2000 |
dc.date.accessioned.fl_str_mv |
2015-01-13T02:14:42Z |
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/10183/108888 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
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000274928 |
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0004-637X 000274928 |
url |
http://hdl.handle.net/10183/108888 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The Astrophysical journal. Chicago. Vol. 539, no. 1, pt. 1 (Aug. 2000), p. 379-391 |
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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