Show simple item record

dc.contributor.authorNicholls, C.P.
dc.contributor.authorWood, P.R.
dc.contributor.authorCioni, M-R.L.
dc.date.accessioned2010-11-30T11:44:12Z
dc.date.available2010-11-30T11:44:12Z
dc.date.issued2010
dc.identifier.citationNicholls , C P , Wood , P R & Cioni , M-RL 2010 , ' Ellipsoidal variability and the difference between sequence D and E red giants ' , Monthly Notices of the Royal Astronomical Society , vol. 405 , no. 3 , pp. 1770-1776 . https://doi.org/10.1111/j.1365-2966.2010.16548.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 181643
dc.identifier.otherPURE UUID: dea613a6-bdf5-4fe1-9da4-71390b84bfbd
dc.identifier.otherdspace: 2299/5035
dc.identifier.otherScopus: 77954916040
dc.identifier.urihttp://hdl.handle.net/2299/5035
dc.descriptionThe definitive version can be found at: http://www3.interscience.wiley.com/ Copyright Royal Astronomical Society
dc.description.abstractWe have studied a sample of Large Magellanic Cloud red giant binaries that lie on sequence E in the period–luminosity plane. We show that their combined light and velocity curves unambiguously demonstrate that they are binaries showing ellipsoidal variability. By comparing the phased light and velocity curves of both sequence D and E variables, we show that the sequence D variation – the long secondary period – is not caused by ellipsoidal variability. We also demonstrate several further differences between stars on sequences D and E. These include differences in velocity amplitude, in the distribution of eccentricity and in the correlations of velocity amplitude with luminosity and period. We also show that the sequence E stars, unlike stars on sequence D, do not show any evidence of a mid-infrared excess that would indicate circumstellar dust.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.titleEllipsoidal variability and the difference between sequence D and E red giantsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2010
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2010.16548.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record