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Observation and Analysis of RW Doradus

Published online by Cambridge University Press:  05 March 2013

B. F. Marino ,
W. S. G. Walker ,
C. Bembrick  and
E. Budding
B. F. Marino
Affiliation:
Auckland Observatory, PO Box 24 180 Royal Oak, Auckland 1345, New Zealand
W. S. G. Walker
Affiliation:
Wharemaru Observatory, Awanui 0552, Kaitaia, New Zealand
C. Bembrick
Affiliation:
Mt. Tarana Observatory, PO Box 1537, Bathurst, NSW 2795, Australia
E. Budding*
Affiliation:
Carter Observatory, PO Box 2909, Wellington, New Zealand & Physics Dept., 18th March University of Canakkale, Turkey
*
ECorresponding author. Email: ebudding@comu.edu.tr
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Abstract

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Photometry of the short-period (P ∼0.285 d) low-mass (M1 ∼0.67, M2 ∼0.48 M⊙) W UMa-type eclipsing binary RW Dor, mainly involving a good series of observations in 1987–88, using standard B and V filters at the Auckland Observatory, is examined. Analysis via light curve fittings alone permits both transit (near main sequence) and occultation (W-type contact binary) solutions. Consideration of proximity or other effects on the relatively small number of measured radial velocities gives rise to a more detailed review of the alternatives, though the (W-type) configuration determined by Hilditch, Hill & Bell (1992) is still confirmed. Further implications of this configuration are examined, given an apparent general trend to period decrease (Δ P/P ∼6 × 10−11), and some light curve asymmetry. This is consistent with the initially low-mass companion, Case-B scenario of Budding (1984). The evidence does suggest irregularity of the period variation however, and further detailed surveillance, including more spectroscopy, is desirable.

Keywords

stars: close binariesstars: late-typestars: individual: RW Dorgeneral: contact binaries techniques: photometric light curve analysis
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 24 , Issue 4 , 2007 , pp. 199 - 207
Copyright
Copyright © Astronomical Society of Australia 2007

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