Abstract
As the first step toward assessing the high-mass end of the PNN (and hence, WD) mass distributions, we report here on new PNN found in extended, low surface brightness PN. Our ultimate goal is to obtain luminosities and temperatures for these stars and to compare them with evolutionary calculations to derive stellar masses. Based on studies of a local sample of PN, Schönberner (1981, 1983) and Schönberner and Weidmann (1983) infer that the PNN mass distribution is sharply peaked near 0.6 M⊙, and that 80% of PNN have masses < 0.61 M⊙. Their sample was necessarily chosen for the existence of photometric data for both the nebulae and their central stars, criteria that excluded small bright PN whose central stars are masked by nebular emission, and large faint PN for which there is little photometric data for the nebulae and/or the central stars. Acknowledging these selection effects, those authors have urged further investigation, especially of low luminosity PNN.
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.
