HL Aurigae: A pre-contact binary system with a solar-mass companion

Abstract

Orbital period changes of the near-contact binary (NCB) system, HL Aurigae, are analyzed based upon all the published CCD and photoelectric times of light minimum. It is found that the period of HL Aurigae shows a small-amplitude cyclic oscillation with a period of 6.5 years and an amplitude of 0. d 0058 while it undergoes a secular decrease at a rate of d P/d t = −1.08 × 10 −7 days/year. The cyclic period oscillation can be interpreted either by the light-time effect of a third body or by magnetic activity cycles of the components. Since the third-body assumption is in agreement with the presence of a large amount of third light in the system discovered by Gray et al. (1997), we think that HL Aurigae may be a true triple system. In order to deduce a G2-type third companion as proposed by Gray et al. (1997), the orbital inclination of the third body should be i′ = 40°, which is much smaller than that of the eclipsing pair ( i = 85.°7). This suggests that the third companion is not coplanar with the eclipsing binary. This may indicate that the solar-mass component may be captured by the eclipsing binary system in some previous stages of its formation and evolution. HL Aurigae is a short-period NCB with a F1V-type primary and a G9V-type secondary component and both of the components are filling or nearly filling their Roche lobes. As the period is decreasing, the shrinking of the Roche lobe will finally cause it to evolve into a contact binary system in the timescale of ∼2.1 × 10 6 years. The period decrease may be caused by mass transfer or/and by angular momentum loss via magnetic braking.