Abstract
ABSTRACTIt has been known since the pioneering work of Eddington & Plakidis that the period changes in Mira stars are dominated by the effects of random cycle‐to‐cycle fluctuations in period, at least in the limited sample of stars that were studied. We have extended their work, using a portion of the American Association of Variable Star Observers (AAVSO) international database of variable star observations: times and magnitudes of maximum and minimum magnitude of 391 bright Mira stars over 75 yr (Kowalsky et al.). The Eddington & Plakidis model fits the data in almost every case, at least over a time interval of several tens of cycles. There is a weak correlation between the fractional period fluctuation, per cycle, and the period (or color) of the star, but not with the amplitude or chemical type (M, S, or C).
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 callMore From: Publications of the Astronomical Society of the Pacific
Disclaimer: 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.
