Abstract
A number of the extended planetary nebulae show point-symmetric morphology, and it has been suggested that such a morphology is the consequence of the episodic ejection of material in a two-sided jet. Here we show that the accretion disk, previously postulated to be formed in the final stages of common envelope evolution giving rise to the planetary nebulae, is unstable to a radiation-induced self-warping instability discovered by Pringle. We show further that the timescales on which the warping instability and concomitant induced precession occur are short enough to be relevant to the planetary nebula ejection process.
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.
