Abstract:
Observations of HR 2947 show that it is fainter by 0.3 mag in V compared to the magnitude listed by Cowley et al. (1969). The energy distribution from 1565 Armstrong to 1.25 micro is similar to that of a B5 III star and does not indicate presence of any companion. Teff ~ 13500 plus or minus 500 K and log g= 3.5 plus or minus 0.5 are obtained by comparison with the theoretical energy distribution. It is suggested that the light variability, if real, could be due to the formation of a thin gas shell around the star.