Orbits of detached main-sequence eclipsing binaries of types late F to K, 1: RT Andromedae and CG Cygni

Details Orbits of detached main-sequence eclipsing binaries of types late F to K, 1: RT Andromedae and CG Cygni Orbits of detached main-sequence eclipsing binaries of types late F to K, 1: RT Andromedae and CG Cygni

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....108.1091p&link_type=abstract

The Astronomical Journal, vol. 108, no. 3, p. 1091-1100

Physics

41

Eclipsing Binary Stars, G Stars, K Stars, Main Sequence Stars, Stellar Mass, Stellar Orbits, Stellar Physics, Stellar Radiation, Stellar Spectra, Astronomical Photometry, Astronomical Spectroscopy, Calibrating, Charge Coupled Devices, Cross Correlation, Graphs (Charts), Spectrum Analysis, Tables (Data)

Scientific paper

A substantial increase of our meager supply of masses and other properties of main-sequence stars in the spectral range late F to K appears to require, because of selection effects, the analysis of eclipsing systems of short period, having spectrum lines badly blended and washed out by rotation. A previous study with synthetic binary spectra has shown that velocities in spectra similar to those of the short-period systems can be obtained relatively free of systematic effects. The spectra employed, obtained with the Hamilton echelle-charge coupled device (CCD) spectrometer at the Lick Observatory, has high dispersion (2.5 km/s per pixel) and signal/noise (70-100 per pixel in the continuum). Analysis is with Interactive Data Reduction and Analysis Facility (IRAF) programs. The first two binaries analyzed in the program are RT And (F8+K3) and CG Cyg (G9+K3), both having periods of 0.63 days. These two are among the very small number of detached short-period binaries with previously published spectroscopic orbits. The orbits of both are shown to be in need of substantial revision. It is of particular interest that another recent (1993) set of velocities for RT And, from spectra also obtained with a linear digital detector and analyzed by a similar cross-correlation procedure, lead to a sum of the masses 22% smaller than obtained from the Lick spectra. I attribute this difference, which demonstrates the need of thorough testing, to the much lower (though respectable) dispersion of the other observations, so that the cross-correlation functions of the two components are not well separated. RT And and CG Cyg have more extensive photometry, more thoroughly analyzed, by M. Zeilik and his collaborators, than other systems. Nevertheless, because of intrinsic variability, attributed to star spots, the radiative properties of the components of the two binaries are not accurately established. That most of the photometric observations are not on a calibrated system contributes to the uncertainties.

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