D. Ballereau and A. M. Hubert, Observatoire de Paris, write: "The Be star HO 58050, of spectral type B2V with stellar low-rotational velocity v sin i = 140 km/s, is known to present strong Balmer emission lines of variable intensity. Spectra taken with the Haute Provence 1.93- and 1.52-m telescopes (dispersions 0.967 and 1.244 x 10**-6) reveal a double Balmer emission centered on a wide photospheric absorption. Emission was visible up to H-12 from 1961 to 1966, with a maximum intensity in 1961. During 1967-1968, there was a minimum of emission, being visible only as far as H-epsilon. The emission was again strengthened and visible to H-11 in 1971 Jan., falling short of the 1961 intensity level. From late 1971 to 1976, emission was weaker but still visible to H-9 and fluctuating in intensity. We have noted a new emission minimum, more significant than that in 1968, on a plate taken on 1980 Nov. 24. A faint double emission feature was visible at H-beta on the wide photospheric absorption, and H-gamma had a diffuse absorption. Independently, J. Busquets, J. Fabregat, L. Rivas, J. C. Misson and A. Figer, Groupe Europeen d'Astronomes Amateurs, observed this star to brighten by 0.5 magnitude, from a mean value of 6.44 during 1979-1980 to 6.00 in 1980 Nov.-Dec. The Balmer emission intensity decrease observed in HD 58050 at the end of 1980 should be strongly correlated with the increase in brightness."
International Astronomical Union Circular
- Pub Date:
- January 1981