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Eccentric Orbits of close Companions to Asymptotic Giant Branch Stars
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I propose that the relatively high eccentricity found in some tidally strongly interacting binary systems, where the mass-losing star is an evolved giant star, e.g., an asymptotic giant branch star, is caused by an enhanced mass loss rate during periastron passages. Tidal interaction by itself will circularize the orbits of these systems in a relatively short time, hence a mechanism which increases the eccentricity on a shorter time scale is required. The proposed scenario predicts that the nebula formed by the mass loss process possesses a prominent departure from axisymmetrical structure. Such a departure is observed in the Red Rectangle, which has a central binary system, HD 44179, with an orbital period of 318 days, and an eccentricity of e=0.38.
Forward citations
Cited by 2 Pith papers
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Reframing the Wide Eccentric Binary Problem: Eccentricity as a Probe of Mass-transfer Physics
Eccentric mass transfer via the new GeMT model accounts for the eccentric orbits of wide sdB+MS binaries as a direct consequence of mass-transfer physics.
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HD 5501: A Rapidly Evolving Interacting Eclipsing Binary with a Variable Light Curve and H$\alpha$ Emission
HD 5501 is an eclipsing binary caught just as its primary begins Roche-lobe overflow, with a rapidly shrinking orbital period and mass loss through the L3 point.
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