U, B, and V light curves by Radhakrishnan et al. (1985) and Hα (wide) and Hα (narrow) light curves by Edalati et al. (1989) of the semi-detached eclipsing binary system R Canis Majoris (R CMa) were analyzed using the Wilson-Devinney synthetic light curve method keeping the two parameters, Te,h (temperature of the hot component) and q (mass-ratio mc/mh) as fixed at 7310 K and 0.158 (Tomkin 1995), respectively. From the results of these analyses the following absolute elements of the system are obtained: mh = 1.070±0.20 Msun, mc = 0.168±0.02 Msun, Rh = 1.50±0.10 Rsun, Rc = 1.15±0.08 Rsun, log Lh/Lsun = 0.76±0.18 and log Lc/Lsun = -0.41±0.16. From the positions of the primary and secondary components in the plots of log m versus log L, log R, and log Te for main sequence stars, it is noticed that both the components are overluminous, oversized, and hotter for their derived masses. Assuming the overluminosity of the primary component to be due to overabundance of He, we calculated the initial masses of the original primary and secondary components of R CMa.
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Sarma et al. (1996) studied this question.