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Limits on planets around pulsating white dwarf stars

dc.contributor.authorMullally, Fergalpt_BR
dc.contributor.authorWinget, Donald Earlpt_BR
dc.contributor.authorDeGennaro, Stevenpt_BR
dc.contributor.authorJeffery, Elizabethpt_BR
dc.contributor.authorThompson, S. E.pt_BR
dc.contributor.authorChandler, Dean W.pt_BR
dc.contributor.authorKepler, Souza Oliveirapt_BR
dc.date.accessioned2015-01-15T02:15:06Zpt_BR
dc.date.issued2008pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/108964pt_BR
dc.description.abstractWe present limits on planetary companions to pulsating white dwarf stars. A subset of these stars exhibit extreme stability in the period and phase of some of their pulsation modes; a planet can be detected around such a star by searching for periodic variations in the arrival time of these pulsations. We present limits on companions greater than a few Jupiter masses around a sample of 15 white dwarf stars as part of an ongoing survey. One star shows a variation in arrival time consistent with a 2MJ planet in a 4.5 yr orbit.We discuss other possible explanations for the observed signal and conclude that a planet is the most plausible explanation based on the data available.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Chicago. Vol. 676, no. 1 (Mar. 2008), p. 573-583pt_BR
dc.rightsOpen Accessen
dc.subjectPulsacoes estelarespt_BR
dc.subjectPlanetary systemsen
dc.subjectAnãs brancaspt_BR
dc.subjectWhite dwarfsen
dc.titleLimits on planets around pulsating white dwarf starspt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000634350pt_BR
dc.type.originEstrangeiropt_BR


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