# Linear nonadiabatic pulsation models of the double-mode Cepheid V371 Per

## TL;DR

This paper models the pulsation behavior of the unique double-mode Cepheid V371 Per, revealing it is likely crossing the instability strip for the first time and highlighting the importance of metallicity and temperature in its pulsation characteristics.

## Contribution

It introduces linear nonadiabatic pulsation models tailored to V371 Per, providing insights into its evolutionary stage and the effects of metallicity on its pulsation properties.

## Key findings

- V371 Per is likely crossing the instability strip for the first time.
- Models require specific mass and Teff ranges that depend on metallicity.
- Observed and model Teff ranges overlap marginally, needing further data.

## Abstract

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.