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dc.contributor.authorDrew, J.E.
dc.contributor.authorJones, D.H.P.
dc.contributor.authorWoods, J.A.
dc.identifier.citationDrew , J E , Jones , D H P & Woods , J A 1993 , ' The donor star of the long-period dwarf nova DX-Andromedae ' , Monthly Notices of the Royal Astronomical Society , vol. 260 , no. 4 , pp. 803-818 .
dc.identifier.otherPURE: 154637
dc.identifier.otherPURE UUID: 5209af32-7fbb-473d-93ee-fe7d44799f72
dc.identifier.otherdspace: 2299/4044
dc.descriptionOriginal article can be found at: Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA]
dc.description.abstractSpectroscopic observations of the long-period dwarf nova DX Andromedae are reported which show that it has a binary period of 0.44167 d, a secondary radial velocity amplitude of 107 km/s, and a projected rotational velocity of 79 km/s. Photometric observations reveal ellipsoidal variation of 0.08 mag in Z. From all the data, it is found that DX And has a mass ratio of 0.96 and that the accretion disk contributes about 15 percent of the light in the green region of the spectrum. The secondary has a spectral type of K1 V and a radius at least 40 percent larger than the corresponding main sequence stars. It is argued that the companion star mass is less than 0.8 solar. The distance to DX And is 630 pc. The secondary star's absorption spectrum does not exactly match that of a normal main-sequence star: enhanced absorption is seen at some wavelengths.en
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectcataclysmic variables
dc.titleThe donor star of the long-period dwarf nova DX-Andromedaeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.typeJournal Article/Review

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