Show simple item record

dc.creatorMukadam, Anjum S.en_US
dc.creatorTownsley, D. M.en_US
dc.creatorSzkody, P.en_US
dc.creatorGansicke, B. T.en_US
dc.creatorWinget, D. E.en_US
dc.creatorHermes, J. J.en_US
dc.creatorHowell, Steve B.en_US
dc.creatorTeske, J.en_US
dc.creatorPatterson, J.en_US
dc.creatorKemp, J.en_US
dc.creatorArmstrong, Eveen_US
dc.date.accessioned2016-10-28T19:38:17Z
dc.date.available2016-10-28T19:38:17Z
dc.date.issued2011-02en_US
dc.identifierdoi:10.15781/T22J6870X
dc.identifier.citationMukadam, Anjum S., D. M. Townsley, Paula Szkody, Boris T. Gänsicke, Donald Earl Winget, J. J. Hermes, Steve B. Howell et al. "First unambiguous detection of the return of pulsations in the accreting white dwarf SDSS J074531. 92+ 453829.6 after an outburst." The Astrophysical Journal Letters, Vol. 728, No. 2 (Feb., 2011): L33.en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/2152/43106
dc.description.abstractThe primary white dwarf of the cataclysmic variable SDSS J074531.92+453829.6 was discovered to exhibit non-radial pulsations in 2006 January. This accreting white dwarf underwent its first recorded dwarf nova outburst in 2006 October, during which its brightness increased by more than 5 mag. A Hubble Space Telescope (HST) ultraviolet spectrum, obtained one year after the outburst, revealed a white dwarf temperature of 16,500 K, hotter than all other known accreting white dwarf pulsators. This implies that the accreting primary white dwarf of SDSS J074531.92+453829.6 was heated to temperatures beyond the instability strip during the outburst. Optical observations acquired a year after the outburst did not reveal any evidence of pulsations, suggesting that the white dwarf had not cooled to quiescence by then. We recently acquired optical high-speed time-series photometry on this cataclysmic variable SDSS J074531.92+453829.6 more than three years after its outburst to find that pulsations have now returned to the primary white dwarf. Moreover, the observed pulsation periods agree with pre-outburst periods within the uncertainties of a few seconds. This discovery is significant because it indicates that the outburst did not affect the interior stellar structure, which governs the observed pulsation frequencies. It also suggests that the surface of the white dwarf has now cooled to quiescence. Using this discovery in addition to the prior HST temperature measurement of 16,500 K, we have been able to constrain the matter accreted during the 2006 outburst. This is the first time an accreting white dwarf was unambiguously observed to resume pulsating after an outburst.en_US
dc.description.sponsorshipNSF AST-0607840, AST-GO-11163.01-A, AST-0908363en_US
dc.description.sponsorshipNASA AST-0607840, HST-GO-11163.01-Aen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectnovae, cataclysmic variablesen_US
dc.subjectstars: dwarf novaeen_US
dc.subjectstars: individualen_US
dc.subject(sdss j074531.92+453829.6)en_US
dc.subjectstars: oscillationsen_US
dc.subjectstars: variables:en_US
dc.subjectgeneralen_US
dc.subjectwhite dwarfsen_US
dc.subjectzz ceti starsen_US
dc.subjecthubble-space-telescopeen_US
dc.subject2001 july outbursten_US
dc.subjectinstabilityen_US
dc.subjectstripen_US
dc.subjectcataclysmic variablesen_US
dc.subjectgw-libraeen_US
dc.subjecteffective temperaturesen_US
dc.subjectopticalen_US
dc.subjectobservationsen_US
dc.subjectlight curvesen_US
dc.subjectspectraen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleFirst Unambiguous Detection of the Return of Pulsations in the Accreting White Dwarf SDSS J074531.92+453829.6 After an Outbursten_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/2041-8205/728/2/l33en_US
dc.contributor.utaustinauthorWinget, D. E.en_US
dc.contributor.utaustinauthorHermes, J. J.en_US
dc.relation.ispartofserialAstrophysical Journal Lettersen_US


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record