Volume 49 number 1 (2021)
In this paper we present our updates and findings surrounding both period and classification analysis of 21 Miras and 4 semiregular variable stars. Our primary methods for confirming pulsation period include both qualitative and quantitative examination of time series plots and light curves, along with cross-confirmation using publicly-accessible databases with over a hundred years of published data. Using the visual observations and the Johnson V data from the AAVSO, and with the help of the AAVSO’s VSTAR software, we arrived at refined period values to confirm data published by the VSX. Somewhat substantial updates are recommended for T UMi, from a period of 115.7 days to a primary and secondary period of 237.5 and 247.6 days, though no other variables merited such sizable adjustments. Finally, the application of self-correlation analysis provided further insight into the cycle-to-cycle changes in period and magnitude of semiregular variables.