Apsidal Motion in the Eclipsing Binary GG Ori

Details Apsidal Motion in the Eclipsing Binary GG Ori Apsidal Motion in the Eclipsing Binary GG Ori

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002arep...46..747v&link_type=abstract

Astronomy Reports, Vol. 46, Issue 9, pp. 747-759

Astronomy and Astrophysics

Astronomy

6

Scientific paper

High-precision WBVR photoelectric observations of the eclipsing binary GG Ori (B9.5V+B9.5V), which has an eccentric orbit (e=0.22), were carried out in 1988 2001 at the Moscow and high-altitude Tian-Shan Observatories of the Sternberg Astronomical Institute. The aim of these observations was investigation of the apsidal motion of the system. Analysis of the resulting 12-year series of observations enabled us for the first time to accurately (to within 11%) measure the rate of rotation of the orbit and to appreciably improve estimates of the photometric and absolute parameters. The observed value of is 28% higher than the theoretical prediction of . The relativistic part of the apsidal motion in this system is a factor of 2.5 greater than the classical term due to the tidal and rotational deformations of the components. The interstellar extinction in the direction of the star (at a distance of r=425 pc) is very large (A v =1.75 m ). A number of recently published results (in particular, the conclusion that the components of this eclipsing binary are young) are confirmed.

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