Volume 388, Number 1, June II 2002
|Page(s)||309 - 319|
|Section||Stellar structure and evolution|
|Published online||28 May 2002|
A revised HRD for individual components of binary systems from BaSeL synthetic photometry
Influence of interstellar extinction and stellar rotation
Observatório Astronómico da Universidade de Coimbra, Santa Clara, 3040 Coimbra, Portugal
Corresponding author: E. Lastennet, firstname.lastname@example.org
Accepted: 19 March 2002
Johnson BVRI photometric data for individual components of binary systems have been provided by ten Brummelaar et al. ([CITE]). This is essential because non-interacting binaries can be considered as two single stars and therefore play a critical role in testing and calibrating single-star stellar evolution sets of isochrones and the implicit theory. While they derived the effective temperature (Teff) from their estimated spectral type, we infer metallicity-dependent Teff from a minimizing method fitting the , and colours. For this purpose, a grid of 621 600 flux distributions were computed from the Basel Stellar Library (BaSeL 2.2) of model-atmosphere spectra, and their theoretical colours compared with the observed photometry. The BaSeL colours show a very good agreement with the BVRI metallicity-dependent empirical calibrations of Alonso et al. ([CITE]), with the temperatures being different by in the range 4000–8000 K for dwarf stars. Before deriving the metallicity-dependent Teff from the BaSeL models, we paid particular attention to the influence of reddening and stellar rotation. We inferred the reddening from two different methods: (i) the MExcessNg code v1.1 (Méndez & van Altena [CITE]) and (ii) neutral hydrogen column density data. A comparison of both methods shows a good agreement for the sample located inside a local sphere of ~500 pc, but we point out a few directions where the MExcess model overestimates the ) colour excess. Influence of stellar rotation on the BVRI colours can be neglected except for 5 stars with large , the maximum effect on temperature being less than 5%. Our final determinations provide effective temperature estimates for each component. They are in good agreement with previous spectroscopic determinations available for a few primary components, and with ten Brummelaar et al. below ~10 000 K. Nevertheless, we obtain an increasing disagreement with their temperatures beyond 10 000 K. Finally, we provide a revised Hertzsprung-Russell diagram (HRD) for the systems with the more accurately determined temperatures.
Key words: stars: fundamental parameters / stars: binaries: visual / stars: abundances / stars: rotation / stars: Hertzsprung-Russell (HR) and C-M diagrams / ISM: dust, extinction
© ESO, 2002
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