Emission Lines in 32 Cygni

Joel A. Eaton

I identify the profusion of emission lines seen in IUE spectra of 32 Cyg (K4-5 Ib+B6-7 IV-V) during total eclipse. With the exception of a very few weak lines, all of these are also seen in zeta Aur during its eclipse, and the stronger features appear in 31 Cyg. Seventy-four percent of these emission lines can be attributed to Fe II. Few are intrisically weaker than gf~0.01. Other spectra definitely present are C II, N I, O I, Si II, Mg II, S II, Cr II, Ni II, Al II, Al III, F III, Si IV, and C IV. No emission lines of the neutral metals, except for fluorescent Fe I UV44, are unambiguously detected; specifically, lines of C I, Si I, or S I were not detected in the spectrum.