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Article: Two new variable sdB stars, HE 0218-3437 and LB 1516

TitleTwo new variable sdB stars, HE 0218-3437 and LB 1516
Authors
KeywordsStars: oscillations
Stars: individual (HE 0218-3437; LB 1516)
Stars: variables: other
Issue Date2010
Citation
Monthly Notices of the Royal Astronomical Society, 2010, v. 401, n. 3, p. 1850-1856 How to Cite?
AbstractWe present photometry which shows that two known hot subdwarf stars, HE 0218-3437 and LB 1516, are variable. LB 1516 exhibits several frequencies in the range 12-25 cycles d-1 (periods of about 1-2 h) with amplitudes less than about 0.003 mag and appears to be a typical slowly pulsating sdB star. Results from a multisite campaign on HE 0218-3437 show the presence of two frequencies only, the lower amplitude variation an apparent subharmonic of the higher amplitude periodicity. It is likely that the star is in a binary system, and that the variability is due to ellipsoidal deformation of the primary star. © 2009 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/208900
ISSN
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DC FieldValueLanguage
dc.contributor.authorKoen, Chris-
dc.contributor.authorKilkenny, David J.-
dc.contributor.authorPretorius, Magaretha L.-
dc.contributor.authorFrew, David J.-
dc.date.accessioned2015-03-23T02:02:07Z-
dc.date.available2015-03-23T02:02:07Z-
dc.date.issued2010-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2010, v. 401, n. 3, p. 1850-1856-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/208900-
dc.description.abstractWe present photometry which shows that two known hot subdwarf stars, HE 0218-3437 and LB 1516, are variable. LB 1516 exhibits several frequencies in the range 12-25 cycles d-1 (periods of about 1-2 h) with amplitudes less than about 0.003 mag and appears to be a typical slowly pulsating sdB star. Results from a multisite campaign on HE 0218-3437 show the presence of two frequencies only, the lower amplitude variation an apparent subharmonic of the higher amplitude periodicity. It is likely that the star is in a binary system, and that the variability is due to ellipsoidal deformation of the primary star. © 2009 RAS.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectStars: oscillations-
dc.subjectStars: individual (HE 0218-3437; LB 1516)-
dc.subjectStars: variables: other-
dc.titleTwo new variable sdB stars, HE 0218-3437 and LB 1516-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2009.15761.x-
dc.identifier.scopuseid_2-s2.0-73949087908-
dc.identifier.volume401-
dc.identifier.issue3-
dc.identifier.spage1850-
dc.identifier.epage1856-
dc.identifier.eissn1365-2966-

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