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- Publisher
- Springer Journals
- Copyright
- Copyright © Pleiades Publishing, Ltd. 2021. ISSN 1990-3413, Astrophysical Bulletin, 2021, Vol. 76, No. 4, pp. 424–434. © Pleiades Publishing, Ltd., 2021. Russian Text © The Author(s), 2021, published in Astrofizicheskii Byulleten’, 2021, Vol. 76, No. 4, pp. 506–516.
- ISSN
- 1990-3413
- eISSN
- 1990-3421
- DOI
- 10.1134/s1990341321040088
- Publisher site
- See Article on Publisher Site
Abstract
An analysis of TESS satellite observations of the AS Cam eclipsing binary has shown that the light of this source pulsates at two frequencies: \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${{\nu }_{1}} = 0.7556$$\end{document} days–1 and \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${{\nu }_{2}} = 0.8658$$\end{document} days–1 with the amplitudes \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${{A}_{1}} = 0_{.}^{{\text{m}}}0110$$\end{document} and \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$${{A}_{2}} = 0_{.}^{{\text{m}}}0087,$$\end{document} correspondingly. Such variations are typical for slowly pulsating B-type stars. We modeled the light curves of AS Cam obtained from 1968 to 2019 to confirm the discovery of a gradual increase in the orbit eccentricity of the system by approximately 0.018 over 50 years. A third light, as one of the light curve solution parameters, on average, amounts to approximately 4% of the total luminosity of the system. For AS Cam this would correspond to an F8–F9-type suggested third body—a main sequence star, the presence of which follows from the light equation of the system. If the third light is a result of a random overlapping of a star unrelated to AS Cam, then the third body may turn out to be a degenerate object or a close binary system. The extremely slow apsidal motion in this system (compared to the value predicted by the standard theory) can be explained by the gravitational influence of a third body with a mass of about \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$1.2{{M}_{ \odot }}$$\end{document} and an orbital inclination of about \documentclass[12pt]{minimal}\usepackage{amsmath}\usepackage{wasysym}\usepackage{amsfonts}\usepackage{amssymb}\usepackage{amsbsy}\usepackage{mathrsfs}\usepackage{upgreek}\setlength{\oddsidemargin}{-69pt}\begin{document}$$70$$\end{document} with respect to the image plane.
Journal
Astrophysical Bulletin – Springer Journals
Published: Oct 1, 2021
Keywords: stars: binaries: eclipsing; stars: individual: AS Cam