Evolutionary and hydrodynamic models of short--period Cepheids

TL;DR

This paper combines evolutionary and hydrodynamic models to study short-period Cepheids, calculating their pulsation periods and period changes, and compares results with recent observations.

Contribution

It presents a novel integrated approach using evolutionary and hydrodynamic models to analyze short-period Cepheids and their period changes.

Findings

Models match observed period change rates for specific Cepheids.

Evolutionary tracks cross the instability strip for stars >5.1 M_sun.

Calculated pulsation periods align with observational data.

Abstract

The evolutionary calculations for population I stars with masses on the main sequence 5 M_\odot <= M_0 <= 6.1 M_\odot and initial fractional abundances of helium Y_0=0.28 and heavier elements Z_0=0.02 were carried out to the stage of central helium exhaustion. Selected core helium--burning models were used as initial conditions for solution of the equations of hydrodynamics and time--dependent convection describing radial pulsations of Cepheids. In the Hertzsprung--Russel diagram the evolutionary tracks are shown to cross the red edge of the instability strip for M_0 > 5.1M_\odot. The grid of hydrodynamic models of core helium--burning Cepheids on the stages of the second and the third crossings of the instability strip was computed. The pulsation period \Pi and the rate of period change \dot\Pi were determined as a continuous function of star age for each evolutionary sequence of first--overtone pulsators. Results of calculations agree with observational estimates of \dot\Pi recently obtained for the short--period Cepheids V532 Cyg, BG Cru and RT Aur.