ABSTRACT
Two multichannel spectral scans and two SIT spectra of the dMe flare star discovered by Bond (1976) are analyzed which were obtained with the 5-m Hale reflector between July 1 and October 28, 1976. It is found that the Balmer lines have a slow gradient, H-beta is strong, the UV spectrum is flat, and the UV excess is about 1 magnitude larger than the average for cool dM stars. An absolute magnitude of about 13.0 is determined along with a distance of 17 pc and a tangential motion (15 km/s) that is characteristic of a young dMe star. It is suggested that 60% to 75% of the radiation above 2.75 inverse microns is either Balmer recombination, nonthermal, or from a hot source. By interpreting the UV excess as an optically thin Balmer-recombination continuum, an electron temperature of about 20,000 K is estimated together with a bolometric luminosity of 2.4 by 10 to the 31st power erg/s and a ratio of 'quiescent' chromospheric continuum to total luminosity that is approximately 1000 times higher than in the sun. It is noted that emission from flare-heated optically thick hot spots could also explain the UV excess.