THE 2 VARIABLES IN THE TRIPLE SYSTEM HR-6469=V819-HER - ONE ECLIPSING, ONE SPOTTED

A complete B V light curve, from 14 nights of good data obtained with the VU-TSU automatic telescope, are presented and solved with the Wils on-Devinney program. Third light is evaluated, with the companion star brighter by 0.58m in V and 0.11m in B. The eclipses are partial. Infe rred color indices yield F2 V and F8 V for the eclipsing pair and G8 I V-III for the distant companion star. After removing the variability d ue to eclipses, we study the residual variability of the G8 IV-III sta r over the ten years 1982 to 1992. Each yearly light curve is fit with a two-spot model. Three relatively long-lived spots are identified, w ith rotation periods of 85.9d, 85.9d, and 86.1d. The weak and intermit tent variability is understood because the G8 IV-III star has a Rossby number at the threshold for the onset of heavy spottedness.