WIRE Satellite Light Curves of Bright Eclipsing Binary Stars

Details WIRE Satellite Light Curves of Bright Eclipsing Binary Stars WIRE Satellite Light Curves of Bright Eclipsing Binary Stars

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..240..268b&link_type=abstract

Binary Stars as Critical Tools and Tests in Contemporary Astrophysics, International Astronomical Union. Symposium no. 240, he

Astronomy and Astrophysics

Astrophysics

Scientific paper

We are undertaking a project to obtain extensive high-precision photometry of bright eclipsing binary stars using the star tracker aboard the WIRE satellite. Our immediate aim is to measure the masses and radii of our target systems to the highest possible accuracy. The resulting physical properties will be excellent tests and calibrators of theoretical models, in particular because several of our targets have very low mass ratios. These data will also allow us to investigate the reliability of eclipsing binary light curve models and limb darkening coefficients, to see just how far such analyses can be pushed. We present a 29-day light curve (sampling rate 15 seconds, with coverage of 30% of each 90-minute Earth orbit of the satellite) of the totally-eclipsing binary Psi Centauri with point-to-point scatter of only 2 mmag. We measure the relative radii of the stars to a precision of 0.2% (random error) from these data, and also find clear evidence for g-mode pulsations in the primary star with amplitudes of only 0.2 mmag. We have also obtained a 25-day light curve of AR Cassiopeiae which will allow us to accurately measure its apsidal motion and the relative radii of the components. In addition to six modulation at the rotational period of the primary star, and several oscillation modes with periods in the range 1--2 days.

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