A complete BV light curve, from 14 nights of good data obtained with the Vanderbilt University-Tennessee State University (VU-TSU) automatic telescope, are presented and solved with the Wilson-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. Inferred color indices yield F2 V and F8 V for the eclipsing pair and G8 IV-III for the distant companion star. After removing the variability due to eclipses, we study the residual variability of the G8 IV-III star 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, with rotation periods of 85.9d, 85.9d, and 86.1d. The weak and intermittent variability is understood because the G8 IV-III star has a Rossby number at the threshold for the onset of heavy spottedness.
van Hamme, W.V.; Hall, D.S.; Hargrove, A.W.; Henry, G.W.; Wasson, R.; Barkslade, W.S.; Chang, S.; Fried, R.E.; Green, C.L.; Lines, H.C.; Lines, R.D.; Nielsen, P.; Powell, H.D.; Reisenweber, R.C.; Rogers, C.W.; Shervais, S.; Tatum, R. "The Two Variables in The Triple System HR 6469=V819 Her: One Eclipsing, One Spotted" Astronomical Journal v.107, p.1521 (1994)