VV Orionis – improved elements |
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Authors: | M B K Sarma P Vivekananda Rao |
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Institution: | (1) Centre for Advanced Study in Astronomy, Osmania University, 500 007 Hyderabad, India |
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Abstract: | TheUBV light curves obtained by Duerbeck (1975) andHa (wide) and Ha (narrow) light curves obtained by Chambliss & Davan (1987) of the detached eclipsing binary VV Orionis (VV
Ori) were analysed using the Wilson-Devinney method fixing the two parametersT
h (25,000 K) and q(0.4172), resulting in the following absolute elements:A = 13.605 ± 0.03 LR⊙,R
h = 5.03 ±0.03R
⊙, Rc = 2.43 ±0.02R
⊙,M
bol,h
= -5.18 ± 0.11,M
bol,c
= -1.54 ± 0.06,m
h
=10.81 + 0.42m
⊙ andm
c
= 4.51 ± 0.41m
⊙. The de-reddened colours obtained from applying the reddening corrections ofE(B-V) = 0m.05 andE(U-B) = O
m
.04, and the derived temperatures of the components, gave spectral types ofB 1.5V for the primary and 54-5V with anUV excess of 0
m
·3 for the secondary component. A comparison of the logL and logT
e of the components with the observed ZAMS shows the primary component to be a little above and the secondary component to
be a little below/or on the ZAMS. A comparison of the properties of the components of VV Ori and a few other detached systems
with the normal stars in the logL, logR and logT
e versus logm planes, indicated a need for either a readjustment of the scales of the above parameters or modifications in the theoretical
models. From the position of the components on the evolutionary tracks of Pop I composition computed by Schaller et al. (1992)
it is noticed that while the primary component of W Ori had slightly evolved along the main-sequence, its secondary is still
unevolved. The age of VV Ori is found to be 10 ± 1 million years and it is at a distance of 368 ± 10 pc. |
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Keywords: | Eclipsing binaries detached VV Ori elements individual |
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