CCD Echelle observations of the active RS CVn system II Pegasi

Optical spectra were obtained of II Peg on eight different nights in 1984 and 1985 to assess the strength and variability of surface activity indicators in this very active RS CVn system. These cross-dispersed echelle spectra covered the range from 390 nm to 900 to 900 nm at a resolution of 12,000. EMission was seen in the first four Balmer lines, in the Ca II infrared triplet, Ca II H lines, and in one observation, in He I D3. The ratio of energy emitted in the H-alpha line to that in H-beta is similar to that in solar prominences, except during enhancements when the ratio decreases toward values more typical of solar flares. The H-alpha lines varied both in strength and in profile. There were slight variations in the Ca II infrared triplet lines. Exposure levels were too weak to assess the variations in H-gamma, H-delta, or Ca II H. Relative to comparison star spectra, the TiO bands at 896 nm and 710 nm were slightly deeper in II Peg, which is indicative of cool spots.