Bond's flare star 2329-03.
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.
- Publication:
-
Publications of the Astronomical Society of the Pacific
- Pub Date:
- June 1977
- DOI:
- 10.1086/130121
- Bibcode:
- 1977PASP...89..304G
- Keywords:
-
- Chromosphere;
- Flares;
- Stellar Spectrophotometry;
- Variable Stars;
- Balmer Series;
- Emission Spectra;
- H Lines;
- Line Spectra;
- Optical Thickness;
- Astrophysics;
- Chromospheres:Flare Stars;
- Flare Stars:Spectrophotometry;
- Flare Stars:Starspots