A model of the Mira-type star T UMi

Abstract

Stellar evolution calculations were carried out from the main sequence to the final AGB stage of stars with initial masses from 1 to $2M_\odot$ and metallicity $Z=0.01$. Selected models of evolutionary sequences were used as initial conditions for solution of the equations of radiation hydrodynamics and time-dependent convection describing radial stellar pulsations. The study was aimed to construct the hydrodynamic models of Mira-type stars that show the secular decrease in the pulsation period commenced in 1970--th at $\Pi=315$ day. We show that such a condition for the period change is satisfied with evolutionary sequences from 1 to $1.2M_\odot$ and the best agreement with observations is obtained for models with initial mass $1.2M_\odot$. The pulsation period reduction is due to both the stellar radius decrease during the thermal pulse of the helium burning shell and mode switch from the fundamental mode to the first overtone. Theoretical estimates of the fundamental parameters of the star at the onset of pulsation period reduction are as follows: the mass is $M=0.93M_\odot$, the luminosity is $L = 4080L_\odot$, and the radius is $R=220R_\odot$. The mode switch occurs 35 years after the onset of period reduction.