And, IM Peg, V711 Tau, II Peg, and VW Cep. The starspot and white light plage contributions and distributions can also be mapped over the surface of the rotating stars by modeling the light, TiO, and color variations. Also, a few Mira and Mira-like variables are being observed. For each night of photometry, the temperatures of the stars are determined from the Wing TiO and near-IR color indices while the relative luminosity of the star is measured from the calibrated 1024nm magnitudes.
Initial results indicate that the red supergiants have different variability characteristics.
Preliminary analysis of the observations shows that the semi-regular light variations of Ori and the other early M supergiants predominantly arise from temperature variations rather from changes in radius. The results of the recent analysis of TV Gem have been completed and will be submitted for publication in early 2001. Papers have already been published for Ori, Her, CE Tau, and V CVn. The TiO-index light curves for this star have been modeled and permit the starspots to be mapped over the star's surface. However, the light curves at the other bandpasses are quite often different from the corresponding TiO-index light curves.