2002A&A...388..309L


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET21:42:08

2002A&A...388..309L - Astronomy and Astrophysics, volume 388, 309-319 (2002/6-2)

A revised HRD for individual components of binary systems from BaSeL BVRI synthetic photometry Influence of interstellar extinction and stellar rotation.

LASTENNET E., FERNANDES J. and LEJEUNE T.

Abstract (from CDS):

Johnson BVRI photometric data for individual components of binary systems have been provided by ten Brummelaar et al. (2000AJ....119.2403T). 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 B-V, V-R and V-I colours. For this purpose, a grid of 621600 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. (1996A&A...313..873A), with the temperatures being different by 3±3% in the range 4000-8000K 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 (Mendez & van Altena, 1998A&A...330..910M) 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 ∼500pc, but we point out a few directions where the MExcess model overestimates the E(B-V) colour excess. Influence of stellar rotation on the BVRI colours can be neglected except for 5 stars with large vsini, 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∼10000K. Nevertheless, we obtain an increasing disagreement with their temperatures beyond 10000 K. Finally, we provide a revised Hertzsprung-Russell diagram (HRD) for the systems with the more accurately determined temperatures.

Abstract Copyright:

Journal keyword(s): stars: fundamental parameters - stars: binaries: visual - stars: abundances - stars: rotation - stars: Hertzsprung-Russell (HR) and C-M diagrams - ISM: dust, extinction

Simbad objects: 29

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Number of rows : 29

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * 85 Peg SB* 00 02 10.3411392575 +27 04 54.476788744 6.47 6.42 5.75 5.16 4.73 G5VbFe-2 529 0
2 * lam Cas ** 00 31 46.3593467 +54 31 20.225689       6.25   B8Vn 132 0
3 HD 13594 ** 02 14 02.45880 +47 29 03.2496       7.00   F4V 142 0
4 * 47 Tau ** 04 13 56.38482 +09 15 49.7729           G5III+A7V: 71 0
5 * r Tau ** 04 23 51.82553 +09 27 39.4939   5.175 5.098     A3V 122 0
6 * 80 Tau ** 04 30 08.59775 +15 38 16.2194   5.887 5.552 5.358 5.161 F0V 173 0
7 HD 30810 ** 04 51 12.5284595938 +11 04 04.881592537   7.322 6.753     F6V 184 1
8 * sig Ori Y*O 05 38 44.7665260139 -02 36 00.284709290 2.54 3.58 3.79 3.87 4.11 O9.5V 754 0
9 * 126 Tau ** 05 41 17.7176759 +16 32 02.925299 4.1 4.709 4.836     B3IV 158 0
10 * 15 Lyn ** 06 57 16.6052608 +58 25 21.940435 5.71 5.20 4.35 3.70 3.26 G5III-IV 114 0
11 * 10 UMa SB* 09 00 38.38067 +41 46 58.6051 4.440 4.390 3.960 3.57 3.35 F3V+G5V 332 0
12 * ksi UMa B SB* 11 18 10.8360115405 +31 31 44.821690914   5.41 4.77 4.4   G2V 329 1
13 * ksi UMa A SB* 11 18 10.901164 +31 31 44.97910   4.79 4.25     F8.5:V 303 1
14 * tet Vir ** 13 09 56.9843568248 -05 32 20.465727623   4.385 4.397     A1IVs 243 0
15 * alf Com A PM* 13 09 59.285492 +17 31 45.85645   5.25 4.80     F5V 237 0
16 * i Boo EB* 15 03 47.29565 +47 39 14.6228           G0Vn 525 0
17 * eta CrB A * 15 23 12.230856 +30 17 17.56212   6.123 5.577     G2V 222 0
18 * gam CrB dS* 15 42 44.56551 +26 17 44.2847           A0V 200 0
19 * lam Oph ** 16 30 54.82314 +01 59 02.1209   3.94 3.90     A1IV 164 0
20 * eta Oph ** 17 10 22.68689 -15 43 29.6639 2.56 2.47 2.42 2.39 2.38 A2IV-V 252 0
21 HD 188405 ** 19 55 19.5002101 -06 44 05.222255   6.86 6.51     F2IV/V 78 0
22 HD 190429 ** 20 03 29.39885 +36 01 30.5082 5.98 6.78 6.63     O4If+O9.5II 198 0
23 HD 193322 ** 20 18 06.98820 +40 43 55.5001 5.17 5.94 5.84 5.69 5.68 O9IV(n)+B1.5V 269 0
24 * bet Del SB* 20 37 32.94130 +14 35 42.3195 4.16 4.07 3.63 3.23 2.99 F5IV 268 0
25 * eta Cap ** 21 04 24.3013240 -19 51 17.971066 5.07 5.02 4.84 4.68 4.61 A5V 108 0
26 * del Equ SB* 21 14 28.8153077 +10 00 25.125878 4.98 4.99 4.49 4.06 3.78 F7(V)+G0(V) 308 0
27 * tau Cyg dS* 21 14 47.49252 +38 02 43.1441 4.140 4.120 3.730 3.38 3.14 F2IV 253 0
28 HD 202908 ** 21 18 34.8827547583 +11 34 07.787823885   7.602 7.013     G0V+G6V 132 0
29 * 37 Peg ** 22 29 57.9401253283 +04 25 54.036511321       6.98   F8(V)+A4(V) 138 0

    Equat.    Gal    SGal    Ecl

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