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Large-Amplitude Ultraviolet Variations in the RR Lyrae Star ROTSE-I J143753.84+345924.8 | | J.M. Wheatley
; B.Y. Welsh
; O.H.W. Siegmund
; Y.I. Byun
; S. Yi
; Y.W. Lee
; B.F. Madore
; M. Viton
; R.M. Rich
; L. Bianchi
; T.A. Barlow
; J. Donas
; K. Forster
; P.G. Friedman
; T.M. Heckman
; P.N. Jelinsky
; R.F. Malina
; D.C. Martin
; B. Milliard
; P. Morrissey
; S.G. Neff
; D. Schiminovich
; T. Small
; A.S. Szalay
; T.K. Wyder
; | | Date: |
10 Nov 2004 | | Journal: | Astrophys.J. 619 (2005) L123 | | Subject: | astro-ph | | Abstract: | The NASA Galaxy Evolution Explorer (GALEX) satellite has obtained simultaneous near and far ultraviolet light curves of the ROTSE-I Catalog RR Lyrae ab-type variable star J143753.84+345924.8. A series of 38 GALEX Deep Imaging Survey observations well distributed in phase within the star’s 0.56432d period shows an AB=4.9mag variation in the far UV (1350-1750A) band and an AB=1.8mag variation in the near UV (1750-2750A) band, compared with only a 0.8mag variation in the broad, unfiltered ROTSE-I (4500-10000A) band. These GALEX UV observations are the first to reveal a large RR Lyrae amplitude variation at wavelengths below 1800A. We compare the GALEX and ROTSE-I observations to predictions made by recent Kurucz stellar atmosphere models. We use published physical parameters for the comparable period (0.57433d), well-observed RR Lyrae star WY Antliae to compute predicted FUV, NUV, and ROTSE-I light curves for J143753.84+345924.8. The observed light curves agree with the Kurucz predictions for [Fe/H]=-1.25 to within AB=0.2mag in the GALEX NUV and ROTSE-I bands, and within 0.5mag in the FUV. At all metallicities between solar and one hundredth solar, the Kurucz models predict 6-8mag of variation at wavelengths between 1000-1700A. Other variable stars with similar temperature variations, such as Cepheids, should also have large-amplitude FUV light curves, observable during the ongoing GALEX imaging surveys. | | Source: | arXiv, astro-ph/0411251 | | Services: | Forum | Review | PDF | Favorites | |
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