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Rediscussion of eclipsing binaries. Paper I. The totally-eclipsing B-type system zeta Phoenicis
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abstract
$\zeta$ Phoenicis is a bright binary system containing B6V and B8V stars. It has deep total and annular eclipses, a slightly eccentric orbit with a period of 1.669 d, apsidal motion and a third body on a wider orbit. The Transiting Exoplanet Survey Satellite light curve and published radial velocities of this system are analysed to determine masses of 3.91 +/- 0.06 Msun and 2.54 +/- 0.03 Msun and radii of 2.84 +/- 0.02 Rsun and 1.89 +/- 0.01 Rsun. The resulting distance to the system is in agreement with its trigonometric parallax. The physical properties of the stars, with the exception of the effective temperature of the secondary component, can be matched by the predictions of several sets of theoretical stellar evolutionary models for a solar chemical composition and an age of 70 to 90 Myr. A spectroscopic analysis of this system is encouraged for the determination of the photospheric chemical composition of the stars, plus improved measurements of their masses and effective temperatures.
Forward citations
Cited by 2 Pith papers
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Pulsating and Non-pulsating Components of Detached Eclipsing Binaries in the $\delta$ Scuti instability strip
Across four detached eclipsing binaries inside the delta Scuti instability strip, the component that does not pulsate is systematically the one with the higher measured metallicity.
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Optical Flares Detected on a Contact Binary: The First Photometric and Spectroscopic Analysis of a Long-period Low Mass Ratio Contact Binary HAT 307-0007476
First study of HAT 307-0007476 reports a low-mass-ratio (q~0.114), medium-contact (f~37%) binary, two superflares, and a gradually increasing orbital period.
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