Abstract
A sample of 33 {[}WR] and wels (weak emission-line central stars) central stars of planetary nebulae was observed in order to search for binary nuclei. One close binary system was discovered. The central star of PN G222.8 - 04.2 is the first {[}WR] star in a close binary system known, with a period of 0.63 d. The fraction of close binary central stars, leading to photometrical variability, is lower among the hydrogen-poor {[}WR] stars and wels than among their hydrogen-rich counterparts. This may indicate larger orbital separations or an intrinsically lower binary fraction among {[}WR] and wels central stars. The detection of one close binary system among the {[}WR] stars shows that common-envelope evolution does not preclude such stars. It also shows that although a stellar merger is a possible evolutionary channel towards H-poor emission-line stars, it cannot form the only such channel, as PN G222.8 - 04.2 has avoided a merger.
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 callDisclaimer: 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.
