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Rediscussion of eclipsing binaries. Paper XXVIII. The metallic-lined system DV Bootes

John Southworth

Abstract

DV Boo is a detached eclipsing binary containing a metallic-lined A-star and a chemically normal late-F star, in an orbit with a period of 3.783 d and a possible slight eccentricity. We use a light curve from the Transiting Exoplanet Survey Satellite (TESS) and published spectroscopic results to determine the physical properties of the system to high precision. We find masses of 1.617 +/- 0.003 Msun and 1.207 +/- 0.004 Msun, and radii of 1.948 +/- 0.008 Rsun and 1.195 +/- 0.022 Rsun. The precision of the radius measurements is limited by the shallow partial eclipses and the unavailability of a spectroscopic light ratio due to the chemical peculiarity of the primary star. We measure a distance to the system of 125.0 +/- 1.5 pc, in good agreement with the Gaia DR3 parallax, and an age of 1.3 Gyr. A comparison with theoretical models suggests the system has a modestly sub-solar metallicity, in conflict with the slightly super-solar photospheric abundances of the secondary star.

Rediscussion of eclipsing binaries. Paper XXVIII. The metallic-lined system DV Bootes

Abstract

DV Boo is a detached eclipsing binary containing a metallic-lined A-star and a chemically normal late-F star, in an orbit with a period of 3.783 d and a possible slight eccentricity. We use a light curve from the Transiting Exoplanet Survey Satellite (TESS) and published spectroscopic results to determine the physical properties of the system to high precision. We find masses of 1.617 +/- 0.003 Msun and 1.207 +/- 0.004 Msun, and radii of 1.948 +/- 0.008 Rsun and 1.195 +/- 0.022 Rsun. The precision of the radius measurements is limited by the shallow partial eclipses and the unavailability of a spectroscopic light ratio due to the chemical peculiarity of the primary star. We measure a distance to the system of 125.0 +/- 1.5 pc, in good agreement with the Gaia DR3 parallax, and an age of 1.3 Gyr. A comparison with theoretical models suggests the system has a modestly sub-solar metallicity, in conflict with the slightly super-solar photospheric abundances of the secondary star.
Paper Structure (8 sections, 5 figures, 4 tables)

This paper contains 8 sections, 5 figures, 4 tables.

Table of Contents

  1. Introduction
  2. DV Boötes
  3. Photometric observations
  4. Light curve analysis
  5. Physical properties and distance to DV Boo
  6. Comparison with theoretical models
  7. Summary and conclusions
  8. Acknowledgements

Figures (5)

  • Figure 1: TESS sector 50 photometry of DV Boo, including only the data analysed in the current work. The flux measurements have been converted to magnitude units and the median subtracted.
  • Figure 2: jktebop best fit to the light curves of DV Boo from TESS sector 50 for the primary eclipse (left panels) and secondary eclipse (right panels). The data are shown as filled red circles and the best fit as a light blue solid line. The residuals are shown on an enlarged scale in the lower panels.
  • Figure 3: RVs of DV Boo compared to the best fit from the jktebop analysis (solid blue lines). The RVs for star A are shown with filled symbols, and for star B with open symbols. The residuals are given in the lower panels separately for the two components. RVs from ÉlodieCarquillat+04mn are shown with red circles, and those from CAOS Catanzaro+24aa with green triangles.
  • Figure 4: Scatter plots of the MC (upper panels) and RP (lower panels) fits for the orbital shape parameters. Blue dotted lines indicate where $e\cos\omega$ and $e\sin\omega$ are zero.
  • Figure 5: Hertzsprung-Russell diagram for the components of DV Boo (filled green circles) and the predictions of the parsec 1.2 models Bressan+12mn. The dashed blue line shows the zero-age main sequence for a metallicity of $Z=0.014$. The dotted blue lines show evolutionary tracks for this metallicity and masses of 1.1$~{\rm M}_\odot$ to 1.7$~{\rm M}_\odot$ in steps of 0.1$~{\rm M}_\odot$ (from bottom-right to top-left). The solid red line shows an isochrone for this metallicity and an age of 1300 Myr.