A direct determination of the parameters for two upper-main sequence stars in the globular cluster omega Centauri

Details A direct determination of the parameters for two upper-main sequence stars in the globular cluster omega Centauri A direct determination of the parameters for two upper-main sequence stars in the globular cluster omega Centauri

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.6806k&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #68.06; Bulletin of the American Astronomical Society, Vol. 30, p.1348

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the first results of a project aimed at the direct determination of the absolute parameters of turn-off stars in nearby globular clusters. The results of our program will allow in turn the determination of ages and distances of globular clusters. We have used the 2.5-m du Pont and and 4-m Blanco telescopes to obtain CCD light and echelle radial velocity curves for OGLEGC-17, a detached eclipsing binary located in the field of omega Centauri. The radial velocity of the system is determined to be -233 km/sec and confirms its cluster membership. Analysis of the eclipse light curves and the radial velocity curves leads to a measurement of the masses and radii of the components of this double-lined binary.The more massive component is just leaving the main-sequence of the cluster. Its mass and radius are m1=0.78 msun and R1=1.87 Rsun. The less massive component is an upper-main sequence star with a mass m2= 0.68 msun and a radius R2=0.89 Rsun.

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