Abstract
Numerical calculations are carried out for the evolution of a binary system with a primary of 5 M⊙ and a secondary of 2 M⊙, revolving round another in a circular orbit of 300 M⊙. After finishing central helium burning, the primary starts to transfer mass to its companion. After the mass loss, the star of originally 5 M⊙ has become a star of 1 M⊙. This star has a carbon-oxygen core which is a well-developed white dwarf, and a very extended hydrogen shell. The final system has a distance of 815 M⊙; the period is 2.3 years.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
Author information
Authors and Affiliations
Editor information
Rights and permissions
Copyright information
© 1969 D. Reidel Publishing Company, Dordrecht, Holland
About this paper
Cite this paper
Lauterborn, D. (1969). White-Dwarf Production in Binary Systems of Large Separation. In: Hack, M. (eds) Mass Loss from Stars. Astrophysics and Space Science Library, vol 13. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3405-0_34
Download citation
DOI: https://doi.org/10.1007/978-94-010-3405-0_34
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-3407-4
Online ISBN: 978-94-010-3405-0
eBook Packages: Springer Book Archive