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Masses of white dwarfs in symbiotic binaries

Published online by Cambridge University Press:  09 October 2020

Kenneth H. Hinkle
Affiliation:
NSF’s National Optical-Infrared Astronomy Research Laboratory, P.O. Box 26732, Tucson, AZ 85726, USA emails: hinkle@noao.edu, joyce@noao.edu
Francis C. Fekel
Affiliation:
Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd, Box 9501, Nashville, TN 37209, USA email: fekel@evans.tsuniv.edu
Richard Joyce
Affiliation:
NSF’s National Optical-Infrared Astronomy Research Laboratory, P.O. Box 26732, Tucson, AZ 85726, USA emails: hinkle@noao.edu, joyce@noao.edu
Thomas Lebzelter
Affiliation:
University of Vienna, Department of Astrophysics, Tuerkenschanzstrasse 17, 1180 Vienna, Austria e-mail: thomas.lebzelter@univie.ac.at
Oscar Straniero
Affiliation:
Istituto Nazionale di Astrofisica, Osservatorio d’Abruzzo, Via Maggini s.n.c., I-64100, Teramo, Italy email: oscar.straniero@inaf.it

Abstract

Masses have been computed for the white dwarfs (WDs) in eclipsing, mass exchange (symbiotic), WD–red giant (RG) binaries by using single-lined spectroscopic orbits, orbital inclinations, and the RG masses. Inclinations have been measured for 13 eclipsing symbiotic binaries. Using Gaia data the mass of the RG can be found from evolutionary tracks. Since the WD evolved from the more massive star in the binary, the WD should be more massive than predicted from the mass of the current RG. Typically the WD has a lower mass than expected implying a previous mass exchange stage for these systems.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

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References

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