Observations of the eclipse in the close binary star BE UMa

Details Observations of the eclipse in the close binary star BE UMa Observations of the eclipse in the close binary star BE UMa

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277...87w&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 1, pp. 87-94.

Astronomy and Astrophysics

Astronomy

17

Binaries: Close, Binaries: Eclipsing, Stars: Fundamental Parameters, Stars: Individual: Be Uma, Stars: Late-Type, Subdwarfs

Scientific paper

We present UBVR photometry of eclipses in the post-common-envelope binary BE UMa. The eclipse is partial in all colours. We fit the eclipses to determine the orbital inclination and the radius of each star. For our best fit we find i=82.˚4+/-0.˚1, R_1/a=0.0781+/-0.0001 and R_2/a=0.138+/-0.001. Using the measured radial velocity of the secondary star, which we correct to account (approximately) for the asymmetric distribution of the line emission, we can calculate the system parameters of the binary for a given mass ratio. We find that for all mass ratios the primary star is a subdwarf and the secondary star lies well inside its Roche lobe. We use the fitted secondary star fluxes to determine its spectral type (G6V-K4V) and hence its mass, 0.69q<0.83. For these limits on q we find 0.83D<1205 pc. The distance of the secondary star is consistent with the primary star's distance if the secondary star has spectral type K3-K4 and hence a distance of ~1230-1071 pc.

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