Constraining stellar physics from red-giant stars in binaries – stellar rotation, mixing processes and stellar activity

¹ Laboratoire AIM Paris-Saclay, CEA/DRF — CNRS — Université Paris Diderot, IRFU/SAp Centre de Saclay, F-91191, Gif-sur-Yvette Cedex, France
² Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria
³ Department of Physics, Faculty of Science, University of Zagreb, Croatia
⁴ LUPM, Université Montpellier II, Place Eugéne Bataillon cc-0072, F-34095, Montpellier cedex 5, France
⁵ Instituut voor Sterrenkunde, KU Leuven, 3001 Leuven, Belgium
⁶ LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris, 92195, Meudon cedex, France
⁷ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
⁸ Departamento de Física Teórica e Experimental, Universidade Federal do Rio

Published online: 27 October 2017

Abstract

The unparalleled photometric data obtained by NASA’s Kepler Space Telescope has led to an improved understanding of stellar structure and evolution - in particular for solar-like oscillators in this context. Binary stars are fascinating objects. Because they were formed together, binary systems provide a set of two stars with very well constrained parameters. Those can be used to study properties and physical processes, such as the stellar rotation, dynamics and rotational mixing of elements and allows us to learn from the differences we find between the two components. In this work, we discussed a detailed study of the binary system KIC 9163796, discovered through Kepler photometry. The ground-based follow-up spectroscopy showed that this system is a double-lined spectroscopic binary, with a mass ratio close to unity. However, the fundamental parameters of the components of this system as well as their lithium abundances differ substantially. Kepler photometry of this system allows to perform a detailed seismic analysis as well as to derive the orbital period and the surface rotation rate of the primary component of the system. Indications of the seismic signature of the secondary are found. The differing parameters are best explained with both components located in the early and the late phase of the first dredge up at the bottom of the red-giant branch. Observed lithium abundances in both components are in good agreement with prediction of stellar models including rotational mixing. By combining observations and theory, a comprehensive picture of the system can be drawn.