The determination of T_eff_ of B, A and F main sequence stars from the continuum between 3200 A and 3600 A.
A method of determination of the effective temperature of B, A and F main sequence stars is proposed, using the slope of the continuum between 3200A and 3600A. The effective temperature calibration is based on a sample of stars with energy distributions known from UV to the red. We have determined the Balmer jump and the effective temperatures for 235 main sequence stars. The temperatures found have been compared with those derived by Underhill et al. (1979), Kontizas & Theodossiou (1980), Theodossiou (1985), Morossi & Malagnini (1985). The comparison showed good agreement for most of the stars in common. On the other hand, the temperatures derived from the reddening-free colour factor QUV, from the colour index (m1965-V) and from (B-V), given in Gulati et al. (1989), are systematically lower than our temperatures, however the differences are within one-sigma error.
Astronomy and Astrophysics Supplement Series
- Pub Date:
- May 1995
- STARS: ATMOSPHERES;
- STARS: EARLY-TYPE;
- STARS: FUNDAMENTAL PARAMETERS