Abstract
Atomic models developed by the author and used to interpret the spectra of cool shells from old classical novae are reviewed. Some of the remaining problems relating to the spectra are discussed briefly. The use of these data in photoionization models is described, and the evolution of nova shells is discussed.
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.
