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Apsidal Motion in Massive Binaries: CPD-41° 7742, an Extreme Case?

Published online by Cambridge University Press:  29 August 2024

S. Rosu Open the ORCID record for S. Rosu [Opens in a new window] ,
G. Rauw ,
Y. Nazé Open the ORCID record for Y. Nazé [Opens in a new window] ,
E. Gosset  and
C. Sterken
S. Rosu*
Affiliation:
STAR Institute, Université de Liège, Allée du 6 août 19c, Bât B5c, 4000 Liège, Belgium
G. Rauw
Affiliation:
STAR Institute, Université de Liège, Allée du 6 août 19c, Bât B5c, 4000 Liège, Belgium
Y. Nazé
Affiliation:
STAR Institute, Université de Liège, Allée du 6 août 19c, Bât B5c, 4000 Liège, Belgium
E. Gosset
Affiliation:
STAR Institute, Université de Liège, Allée du 6 août 19c, Bât B5c, 4000 Liège, Belgium
C. Sterken
Affiliation:
Physics Department, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium
*
email: sophie.rosu@uliege.be
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Abstract

We study the apsidal motion in close eccentric massive binaries. Measuring the rate of apsidal motion in such a system gives insight into the internal structure and evolutionary state of the stars. We focus on CPD-41° 7742, for which independent studies in the past showed large discrepancies in the longitude of periastron of the orbit, hinting at the presence of apsidal motion. We perform a consistent analysis of all observational data to solve this apparent discrepancy and report the first determination of apsidal motion in this system. This study confirms the need for enhanced mixing in the stellar evolution models of the primary star to reproduce the observational properties. This points towards larger convective cores than usually considered.

Keywords

Stars: early-typeevolutionmassiveBinaries: spectroscopiceclipsing
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 248 - 250
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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