  Recently found double-mode Cepheid with the shortest period in our galaxy and
abnormal period ratio, V371 Per is investigated by linear nonadiabatic
pulsation models. V371 Per is likely to be crossing the instability strip for
the first time because mass derived from pulsation models is larger than the
evolution mass for the second or higher crossing objects. This result seems to
support the conclusion obtained from the spectroscopic observation. We also
found that models with observed period and period ratio of V371 Per need to
have mass and Teff in a narrow range which shifts as heavy element abundance Z
changes. We have checked the agreement between Teff ranges estimated
observationally and derived from pulsation models using observational Z. We
found that those ranges overlap marginally. We need more spectroscopic
estimations of the Teff and [Fe/H], and more photometric monitoring to estimate
the evolutionally period change for confirmation of our result.
