# 1997A&A...327.1094V

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 Query : 1997A&A...327.1094V

1997A&A...327.1094V - Astronomy and Astrophysics, volume 327, 1094-1106 (1997/11-3)

V 3903 Sagittarii: a massive main-sequence (O7V+O9V) detached eclipsing binary.

VAZ L.P.R., CUNHA N.C.S., VIEIRA E.F. and MYRRHA M.L.M.

Abstract (from CDS):

We present for the first time an analysis based on uvby light curves, Hβ indices and on new spectroscopic data of the massive detached double-lined O-type eclipsing binary V 3903Sgr. The uvby light curves are analysed with the WINK (initial solutions) and the Wilson-Devinney (WD, final solution) programs. Both codes were used in their extended versions, with stellar atmospheres and taking into account the geometric distortions and photometric effects caused by proximity of the components. The spectroscopic CCD observations were analysed with the harmonic Wilsing-Russell'' and the Lehman-Filhes'' methods. We conclude that V 3903Sgr is one of the rare O-type detached systems where both components are still on the initial phases of the main sequence, with an age of either 1.6x106yrs or 2.5x106yrs (depending on the evolutionary model adopted) at a distance of ≃1500pc, the same as for the Lagoon Nebula (Messier 8) complex, of which the system is probably a member. We determine the absolute dimensions: MA=27.27±0.55, RA=8.088±0.086, MB=19.01±0.44 and RB=6.125±0.060 (solar units). There is no evidence of mass transfer and the system is detached. The orbit is circular, and both components show synchronous rotation, despite their early evolutionary stage. The absolute dimensions determined should be representative for normal single stars. Amongst the massive systems (M>17M) with precise absolute dimensions (errors <2%), V3903 Sgr is that with the most massive primary, with the largest mass difference between the components, and it is the youngest one.

Journal keyword(s): binaries: eclipsing - stars: individual: V3903 Sgr - early type - fundamental parameters

 Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* EM Car EB* 11 12 04.5060592584 -61 05 42.944560584 8.06 8.80 8.54 9.25   O7.5V((f))+O7.5V((f)) 156 0
2 V* LZ Cen EB* 11 50 32.4607560408 -60 47 38.037891264   8.28 8.25 9.02   B2III 46 0
3 * del Sco SB* 16 00 20.00528 -22 37 18.1431 1.30 2.20 2.32 2.36 2.49 B0.3IV 717 0
4 * tau Sco * 16 35 52.9528530 -28 12 57.661515 1.55 2.56 2.81 2.93 3.18 B0.2V 887 0
5 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1774 2
6 * gam Ara Be* 17 25 23.6593111 -56 22 39.814775 2.25 3.21 3.34     B1Ib 264 0
7 V* V906 Sco EB* 17 53 54.7731227 -34 45 09.785378   5.95 5.96     B9V+B9V 120 0
8 * 7 Sgr * 18 02 51.0986253456 -24 16 56.882232732   5.86 5.34     F2II-III 70 0
9 NGC 6523 Cl* 18 03.2 -24 23           ~ 185 1
10 HD 164681 * 18 03 23.8001948376 -26 19 11.367672996   7.40 7.33     A0III/IV 9 0
11 M 8 HII 18 03 37 -24 23.2           ~ 582 1
12 HD 164865 s*b 18 04 15.2161048560 -24 11 00.078860400 8.62 8.470 7.630 6.74 5.910 B9Ia 64 0
13 NGC 6530 OpC 18 04 31 -24 21.5           ~ 381 0
14 * 11 Sgr Or* 18 09 17.6999100192 -23 59 18.231196056 6.65 7.45 7.31 8.36   O7V(n)z+B0:V: 133 2
15 IC 4685 ISM 18 09.3 -23 59           ~ 4 0
16 HD 165999 * 18 09 36.2704295400 -23 34 04.682698932 8.13 7.91 7.64     A2IV 13 0
17 HD 167666 * 18 17 24.0863321904 -28 39 07.435556856   6.350 6.168     A5V 28 0
18 V* Y Cyg SB* 20 52 03.5771840640 +34 39 27.486121104 6.31 7.23 7.32     O9.5IV+O9.5IV 361 1
19 HD 215835 SB* 22 46 54.1107754872 +58 05 03.533752788 8.24 8.85 8.629   8.049 O5.5V((f))+O6V((f)) 245 0

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2022.05.24-09:06:22