Abstract
ABSTRACT Statistical considerations indicate that a nonnegligible fraction of apparently single mainsequence stars earlier than AS should actually be the more massive components of binaries in which a large-scale mass exchange has occurred (van den Heuvel 1969). It is rather difficult to identif these objects. If the -mechanism as proposed by Stothers and Simon (1969) were the correct explanation of the fi Cephei phenomenon, then this phenomenon would identify one class of these transformed binaries. From known models of mass exchange, some conditions are derived that should be fulfilled by binaries if they are to display the -mechanism. Most of the stars in the list by Stothers and Simon (1970) do not seem to meet these conditions. If some of them are found to be P Cep variables, then either the -mechanism or the models of mass exchange will have to be revised. It is suggested that certain peculiar binaries and shell stars (and possibly also symbiotic variables) are binaries observed at the stage of mass exchange or mass loss. Key words: P Cephei variable stars - mass exchange
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callMore From: Publications of the Astronomical Society of the Pacific
Disclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
