AR Lacertae
Star system in the constellation Lacerta
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Observation history
The variability of this binary system was discovered by H. R. Leavitt at Harvard College Observatory, and announced in August 1907 by E. C. Pickering. Due to an orbital period of nearly two days, the eclipsing binary nature of this system was not recognized until 1929 by L. G. Jacchia. W. E. Harper derived orbital elements in 1933. It has an orbital period of 1.98 days and a brightness variation of 0.06 in visual magnitude.
In 1934, A. B. Wyse published spectral classes of K0 and G5 for the components. The K0 star displayed sharp emission lines of singly ionized calcium. The primary minimum is caused by the larger K0 component eclipsing the hotter G5 star, while the secondary eclipse is an annular eclipse of the K0 component by the smaller companion. The stars displayed periodic light variations indicating ellipticity and reflection. The K0 star also showed evidence of significant limb darkening.
In 1946, F. B. Wood reported the intrinsic variability of the hotter component. This variation only disappeared when the smaller star was being eclipsed. The following year, G. E. Kron hypothesized that this variation was due to the presence of huge light and dark patches on the star. To explain the light variations, these had to cover about 20% of the total visible surface, and they must form, move, and later dissolve. The variation was modulated by the rotation period of the star.
By 1972, AR Lac had been identified as an RS Canum Venaticorum variable (RS CVn), consisting of two subgiant stars in a detached binary system. It was found to be a source for radio emission in 1973. This emission varied over time and the system displayed flare activity. The system was detected as an X-ray source by EXOSAT in 1987. The X-ray source with a temperature of 5–7 million K dropped to a minimum during the primary eclipse, indicating it originated on the hotter star. In contrast, X-ray emission from 15–30 million K plasma was not eclipsed, indicating a source larger than the two stars.
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Properties
This is a close, double-lined spectroscopic binary star system, which means the spectra of both components are visible and overlap. They have an essentially circular orbit with a period of 1.98395 days and a separation of 8.9 times the radius of the Sun. The orbital plane is inclined at an angle of 90° to the plane of the sky, which is why two eclipses are visible every orbit. As with other RS CVn systems, their rotation periods are tidally locked to their orbital period. The cooler component is the larger and more massive star, which is consistent with its evolutionary state. There is some evidence of extended matter around this star.
Both components display star spots with an activity cycle of about 17 years. Variation in the orbital period of this system has been reported since 1998, which shows a cyclical oscillation over a period of 50.93 years, and a long-term decrease of a day every 470 million years. This orbital variation may be the result of magnetic activity of the two stars. Stellar flares radiate at a temperature of 12,000±300 K and expand to 2% of the stellar surface.
In 2022, a co-moving companion to this system was announced, making this a triple star system. It was discovered by the Backyard Worlds: Planet 9 citizen science project. Designated WDJ220838.73+454434.04, this companion is a white dwarf at an angular separation of 21.9″ from the binary pair. At the distance of AR Lac, this is equivalent to a projected separation of about 930 AU. It has a mass of 0.6+0.04
−0.09 M☉ and a radius of 0.0125+0.0014
−0.0012 R☉. The companion has an estimated age of 5.75 Gyr and has been steadily cooling for about the last 1.62 Gyr. As a main sequence star, it had a mass of 1.34+0.46
−0.27 M☉. At the estimated separation, a circular orbit of this companion around the inner binary would have an orbital period of approximately 16,000 years.