Marino, B. F.Walker, W. S. G.Bembrick, C.Budding, E.2025-01-272025-01-2720071323-3580https://doi.org/10.1071/AS07009https://hdl.handle.net/20.500.12428/27539Photometry of the short-period (P similar to 0.285 d) low-mass (M-1 similar to 0.67, M-2 similar to 0.48 M-circle dot) 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 (Delta P/P similar to 6 x 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.eninfo:eu-repo/semantics/openAccessstars : close binariesstars : late-typestars : individual : RW Dorgeneral : contact binaries techniques : photometric light curve analysisArticle24419920710.1071/AS07009Q3WOS:0002514280000032-s2.0-36849052889Q1