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Article: Two new young, wide, magnetic + non-magnetic double-degenerate binary systems

TitleTwo new young, wide, magnetic + non-magnetic double-degenerate binary systems
Authors
KeywordsStars: magnetic fields
White dwarfs
Binaries:general
Issue Date2012
Citation
Monthly Notices of the Royal Astronomical Society, 2012, v. 421, n. 1, p. 202-212 How to Cite?
AbstractWe report the discovery of two, new, rare, wide, double-degenerate binaries that each contain a magnetic and a non-magnetic star. The components of SDSSJ092646.88+132134.5 + J092647.00+132138.4 and of SDSSJ150746.48+521002.1 + J150746.80+520958.0 have angular separations of only 4.6 arcsec (a~ 650au) and 5.1 arcsec (a~ 750au), respectively. They also appear to share common proper motions. Follow-up optical spectroscopy has revealed each system to consist of a DA and a H-rich high-field magnetic white dwarf (HFMWD). Our measurements of the effective temperatures and the surface gravities of the DA components reveal both to have larger masses than is typical of field white dwarfs. By assuming that these degenerates have evolved essentially as single stars, owing to their wide orbital separations, we can use them to place limits on the total ages of the stellar systems. These suggest that in each case the HFMWD is probably associated with an early-type progenitor (M init > 2M ⊙). We find that the cooling time of SDSSJ150746.80+520958.0 (DAH) is lower than might be expected had it followed the evolutionary path of a typical single star. This mild discord is in the same sense as that observed for two of the small number of other HFMWDs for which progenitor mass estimates have been made, REJ0317-853 and EG59. The mass of the other DAH, SDSSJ092646.88+132134.5, appears to be smaller than expected on the basis of single-star evolution. If this object was/is a member of a hierarchical triple system it may have experienced greater mass loss during an earlier phase of its life as a result of its having a close companion. The large uncertainties on our estimates of the parameters of the HFMWDs suggest that a larger sample of these objects is required to firmly identify any trends in their inferred cooling times and progenitor masses. This should shed further light on their formation and on the impact magnetic fields have on the late stages of stellar evolution. To serve as a starting point, we highlight two further candidate young, wide magnetic + non-magnetic double-degenerate systems within SDSS, CBS229 and SDSSJ074853.07+302543.5 + J074852.95+302543.4, which should be subjected to detailed (resolved) spectroscopic follow-up studies. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/208934
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806

 

DC FieldValueLanguage
dc.contributor.authorDobbie, Paul D.-
dc.contributor.authorBaxter, R. B.-
dc.contributor.authorKülebi, Baybars-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorKoester, Detlev-
dc.contributor.authorJordan, Stefan M.-
dc.contributor.authorLodieu, Nicolas-
dc.contributor.authorEuchner, Fabian-
dc.date.accessioned2015-03-23T02:02:14Z-
dc.date.available2015-03-23T02:02:14Z-
dc.date.issued2012-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2012, v. 421, n. 1, p. 202-212-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/208934-
dc.description.abstractWe report the discovery of two, new, rare, wide, double-degenerate binaries that each contain a magnetic and a non-magnetic star. The components of SDSSJ092646.88+132134.5 + J092647.00+132138.4 and of SDSSJ150746.48+521002.1 + J150746.80+520958.0 have angular separations of only 4.6 arcsec (a~ 650au) and 5.1 arcsec (a~ 750au), respectively. They also appear to share common proper motions. Follow-up optical spectroscopy has revealed each system to consist of a DA and a H-rich high-field magnetic white dwarf (HFMWD). Our measurements of the effective temperatures and the surface gravities of the DA components reveal both to have larger masses than is typical of field white dwarfs. By assuming that these degenerates have evolved essentially as single stars, owing to their wide orbital separations, we can use them to place limits on the total ages of the stellar systems. These suggest that in each case the HFMWD is probably associated with an early-type progenitor (M init > 2M ⊙). We find that the cooling time of SDSSJ150746.80+520958.0 (DAH) is lower than might be expected had it followed the evolutionary path of a typical single star. This mild discord is in the same sense as that observed for two of the small number of other HFMWDs for which progenitor mass estimates have been made, REJ0317-853 and EG59. The mass of the other DAH, SDSSJ092646.88+132134.5, appears to be smaller than expected on the basis of single-star evolution. If this object was/is a member of a hierarchical triple system it may have experienced greater mass loss during an earlier phase of its life as a result of its having a close companion. The large uncertainties on our estimates of the parameters of the HFMWDs suggest that a larger sample of these objects is required to firmly identify any trends in their inferred cooling times and progenitor masses. This should shed further light on their formation and on the impact magnetic fields have on the late stages of stellar evolution. To serve as a starting point, we highlight two further candidate young, wide magnetic + non-magnetic double-degenerate systems within SDSS, CBS229 and SDSSJ074853.07+302543.5 + J074852.95+302543.4, which should be subjected to detailed (resolved) spectroscopic follow-up studies. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectStars: magnetic fields-
dc.subjectWhite dwarfs-
dc.subjectBinaries:general-
dc.titleTwo new young, wide, magnetic + non-magnetic double-degenerate binary systems-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2012.20291.x-
dc.identifier.scopuseid_2-s2.0-84858007738-
dc.identifier.volume421-
dc.identifier.issue1-
dc.identifier.spage202-
dc.identifier.epage212-
dc.identifier.eissn1365-2966-

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