2003A&A...402..667D


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.26CET02:06:33

2003A&A...402..667D - Astronomy and Astrophysics, volume 402, 667-682 (2003/5-1)

Gravity-darkening exponents in semi-detached binary systems from their photometric observations: Part I.

DJURASEVIC G., ROVITHIS-LIVANIOU H., ROVITHIS P., GEORGIADES N., ERKAPIC S. and PAVLOVIC R.

Abstract (from CDS):

From the light curve analysis of several semi-detached close binary systems, the exponent of the gravity-darkening (GDE) for the Roche lobe filling components has been empirically estimated. The analysis, based on Roche geometry, has been made using the latest improved version of our computer programme. The present method of the light-curve analysis enables simultaneous estimation of the systems' parameters and the gravity-darkening exponents. The reliability of the method has been confirmed by its application to the artificial light curves obtained with a priori known parameters. Further tests with real observations have shown that in the case of well defined light curves the parameters of the system and the value of the gravity-darkening exponent can be reliably estimated. This first part of our analysis presents the results for 9 of the examined systems, that could be briefly summarised as follows: 1) For four of the systems, namely: ZZ Cru, RZ Dra, XZ Sgr and W UMi, there is a very good agreement between empirically estimated and theoretically predicted values for purely radiative and convective envelopes. 2) For the rest five, namely: TT Aur, V Pup, TV Cas, LT Her, and VV UMa, the estimated values of the gravity-darkening exponents were deduced to be larger than theory expects for purely radiative or convective envelopes, respectively. Moreover, it is worthwhile to mention that these values -although greater than theoretical predictions- are: a) Smaller compared to those found by others. b) In two cases, (TV Cas & LT Her), they are normal if some kind of solar type activity (i.e. by employing the Roche model involving a spotted area on the surface of the secondary star) is assumed. 3) The large values derived for the two early type systems TT Aur & V Pup, are very possibly connected with the effects of rotation laws, and in some degree with the large contribution of the radiative pressure in the total potential, leading by that to considerable deviations of the stellar surfaces from the assumed classical Roche geometry. 4) Finally, in the VV UMa case, the estimated value of the gravity-darkening exponent - although almost double than the expected for stars with convective envelopes - still it is low in comparison with that estimated by others who have analysed the same data. But, since for this particular binary the anomalous GDE is not supported by recent simultaneous uvby observations (Lazaro et al., 2001MNRAS.325..617L]), the estimated higher value may be due to the old observational material used.

Abstract Copyright:

Journal keyword(s): stars: general - binaries: close - stars: fundamental parameters - stars: general

Simbad objects: 9

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Number of rows : 9

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 V* TV Cas Al* 00 19 18.7424190416 +59 08 20.541942509 7.27 7.29 7.22     B9V 266 0
2 V* TT Aur bL* 05 09 42.2876514730 +39 35 10.736742938 8.65 8.668 8.602     B2Vn 131 0
3 V* V Pup bL* 07 58 14.4391988 -49 14 41.680272 3.28 4.24 4.41     B1Vp+B2: 229 0
4 V* VV UMa Al* 09 38 06.7194183867 +56 01 07.289041687   10.42 10.28 10.135   A2V 129 0
5 V* ZZ Cru bL* 12 05 45.3865080170 -63 30 14.567730377   9.74 9.76     B3V 25 0
6 V* W UMi Al* 16 08 27.2727942531 +86 11 59.551056069   8.92 8.65     A2V 111 0
7 V* LT Her Al* 16 50 20.4469761305 +09 56 51.865792147   10.63 10.55     A1 41 0
8 V* XZ Sgr Al* 18 22 06.7704634239 -25 14 23.840994391   9.29 8.94     A2/3(IV) 83 0
9 V* RZ Dra EB* 18 23 05.4108271920 +58 54 12.825118885   10.55 10.31     A6V 121 0

    Equat.    Gal    SGal    Ecl

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2021.02.26-02:06:33

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