Short-Period Noncontact Close Binary Systems. VI. V392 Orionis

Abstract

Abstract Photometric and spectroscopic observations in the optical region of the short-period eclipsing binary system V392 Ori (A5 V, $P = 0.6593 \,\mathrm{d}$) were performed and light and radial velocity curves were obtained. The light curves taken at various times are slightly different from one another. Analyses of the light and radial velocity curves yielded photometric and spectroscopic elements of the system. The derived mass function is quite small, $f(M) = 0.0108 \,{{{M}_{\odot}}}$. The masses of the primary and secondary components were found to be 1.2${M}_{\odot}$ and 0.3${M}_{\odot}$, respectively, and the radii are 1.7${R}_{\odot}$ and 0.9${R}_{\odot}$. V392 Ori was found to belong to a group of low-mass binary systems. Due to the semidetached nature of the system, the loss of mass/angular momentum from the system may occasionally occur, inducing a probable effect on the light curves of the system. We compare the system with other low-mass binary systems and discuss the evolutionary status of the system.