2022A&A...666A.128G


Query : 2022A&A...666A.128G

2022A&A...666A.128G - Astronomy and Astrophysics, volume 666A, 128 (2022/10-1)

Surface brightness-colour relations of dwarf stars from detached eclipsing binaries I. Calibrating sample.

GRACZYK D., PIETRZYNSKI G., GALAN C., SOUTHWORTH J., GIEREN W., KALUSZYNSKI M., ZGIRSKI B., GALLENNE A., GORSKI M., HAJDU G., KARCZMAREK P., KERVELLA P., MAXTED P.F.L., NARDETTO N., NARLOCH W., PILECKI B., PYCH W., ROJAS GARCIA G., STORM J., SUCHOMSKA K., TAORMINA M. and WIELGORSKI P.

Abstract (from CDS):


Aims. Surface brightness - colour relations (SBCRs) are very useful tools for predicting the angular diameters of stars. They offer the possibility to calculate very precise spectrophotometric distances by the eclipsing binary method or the Baade-Wesselink method. Double-lined Detached Eclipsing Binary stars (SB2 DEBs) with precisely known trigonometric parallaxes allow for a calibration of SBCRs with unprecedented precision. In order to improve such calibrations, it is important to enlarge the calibration sample of suitable eclipsing binaries with very precisely determined physical parameters.
Methods. We carefully chose a sample of ten SB2 DEBs in the solar neighbourhood which contain inactive main-sequence components. The components have spectral types from early A to early K. All systems have high-precision parallaxes from the Gaia mission. We analysed high precision ground- and space-based photometry simultaneously with the radial velocity curves derived from HARPS spectra. We used spectral disentangling to obtain the individual spectra of the components and used these to derive precise atmospheric parameters and chemical abundances. For almost all components, we derived precise surface temperatures and metallicities.
Results. We derived absolute dimensions for 20 stars with an average precision of 0.2% and 0.5% for masses and radii, respectively. Three systems show slow apsidal motion. One system, HD 32129, is most likely a triple system with a much fainter K6V companion. Also three systems contain metallic-line components and show strong enhancements of barium and ittrium.
Conclusions. The components of all systems compare well to the SBCR derived before from the detached eclipsing binary stars. With a possible exception of HD 32129, they can be used to calibrate SBCRs with a precision better than 1% with available Gaia DR3 parallaxes.

Abstract Copyright: © D. Graczyk et al. 2022

Journal keyword(s): binaries: spectroscopic - binaries: eclipsing - stars: fundamental parameters - stars: distances

VizieR on-line data: <Available at CDS (J/A+A/666/A128): table1.dat table2.dat table4.dat>

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7084 0
2 V* TZ For SB* 03 14 40.0925678952 -35 33 27.594929088   7.620 6.878     F7III+G8III 133 0
3 HD 26590 PM* 04 11 34.3061966592 -20 20 26.398909248   7.97 7.64     F0V 15 0
4 V* GW Eri SB* 04 11 36.2037143376 -20 21 22.156679988 6.05 5.96 5.80 5.64 5.59 A1V+(F/G) 77 0
5 HD 32129 * 05 01 28.2844016208 +15 05 28.678313832   9.62 9.09     F5V 4 0
6 HD 91546 PM* 10 34 43.7465258472 +26 09 32.105756520   8.28 7.81     F5 25 0
7 V* UW LMi SB* 10 43 30.2042029080 +28 41 09.086259732   8.90 8.32     G0V(N) 41 0
8 * 45 LMi * 10 52 48.8484114024 +27 51 54.739165356   7.90 7.47     F5 29 0
9 HD 94426 PM* 10 54 25.5473978472 +30 31 55.120155996   8.08 7.55     F8V 29 0
10 V* QR Hya SB* 10 56 31.1510369784 -34 33 50.152797252   9.63 8.399   7.706 G1V 38 0
11 V* FM Leo SB* 11 12 45.0946779024 +00 20 52.843463628   8.95 8.45 8.89   F7V 51 0
12 V* V788 Cen SB* 12 08 53.8008318648 -44 19 33.563648280   5.991 5.746     A2mA5-F2 57 0
13 HD 114250 PM* 13 10 22.4788847088 -57 44 40.114335804   8.16 7.66     F5IV/V 25 0
14 V* V338 Vir EB* 13 11 17.4072040896 -11 06 21.256937064   9.614 9.130     F5V 11 0
15 HD 115031 PM* 13 15 20.5133822208 -55 20 29.728277268   8.98 8.34     G2/3V 58 0
16 V* V963 Cen SB* 13 18 44.3568297792 -58 16 01.258922892   9.24 8.59     G2V 38 0
17 HD 117214 * 13 30 08.9748682296 -58 29 04.356014100   8.55 8.06     F6V 69 1
18 V* LX Mus SB* 13 40 11.5292231136 -74 04 44.976937512   9.30 8.79     F5V 23 0
19 V* V362 Pav EB? 18 49 03.4801097040 -63 16 10.299206568   7.59 7.41     A2mA5-A9 24 0
20 V* CQ Ind EB* 21 31 03.2887240704 -50 50 48.909314904   8.889 8.35     F7V 27 0

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