Contact and near-contact binary systems. IV - RT Scl and AQ TUC

Details Contact and near-contact binary systems. IV - RT Scl and AQ TUC Contact and near-contact binary systems. IV - RT Scl and AQ TUC

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.223..581h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 223, Dec. 1, 1986, p. 581-593. SERC-supported research.

Astronomy and Astrophysics

Astronomy

37

Eclipsing Binary Stars, Stellar Spectra, Astronomical Spectroscopy, Ephemerides, Light Curve, Radial Velocity, Stellar Luminosity, Stellar Orbits

Scientific paper

Reticon spectroscopic observations are presented for the short-period eclipsing binary systems RT Scl and AQ Tuc. Analysis of these data together with new analyses of previously published light curves show that RT Scl is composed of a main-sequence primary component, virtually in contact with its Roche lobe, and a detached secondary component which is ≡40 per cent larger than expected for its mass. The observed decrease in orbital period and the asymmetry in the light curve may be understood in terms of mass transfer from the primary component at a rate of 10-8M_sun;yr-1 via a stream from the inner Lagrangian point which hits directly the surface of the oversized secondary. The system AQ Tuc, which has the same total mass and specific orbital angular momentum as RT Scl, is confirmed to be an A-type W UMa contact system. There is some disagreement between the spectroscopic and photometric determinations of the mass ratio. The best solutions of the light curves are obtained with a convective value (β = 0.03) for the gravity-darkening exponent. These findings support the conclusions reached by Eaton that convective (or turbulent) atmospheres extend to earlier spectral types amongst contact systems than amongst single stars.

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