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A recently presented HST/FGS parallax measurement of the Polaris system hasbeen interpreted as evidence for the Cepheid Polaris Aa to be pulsating in thesecond overtone. An age discrepancy between components A and B has been notedand discussed in terms of a stellar merger. Here I show that the new parallaxof Polaris is consistent with a simpler interpretation of Polaris as a $7\rm{M}_\odot,$ first-overtone, classical Cepheid near the hot boundary of thefirst instability strip crossing. This picture is anchored to rates of periodchange, the period-luminosity relation, the location in color-magnitude space,the interferometrically determined radius, spectroscopic N/C and N/Oenhancements, and a dynamical mass measurement. The detailed agreement betweenmodels and data corroborates the physical association between the Cepheid andits visual companion as well as the accuracy of the HST parallax. The agediscrepancy between components A and B is confirmed and requires furtheranalysis, for example to investigate the possibility of stellar mergers in anevaporating birth cluster of which the Polaris triple system would be theremaining core.

Homing in on Polaris: A 7 M$_\odot$ first-overtone Cepheid entering the instability strip for the first time