Abstract
AbstractAfter the main-sequence the evolution of stars begins to depend more and more on their initial mass. The discussion of post-main sequence evolution is therefore best split into different mass ranges. We begin with the intermediate mass range and the evolution through the second major burning phase, core helium burning. Typical representatives of this phase and mass range are the classical Cepheids.KeywordsMain SequenceStellar MassHydrogen BurningEvolutionary TrackConvective CoreThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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.
