Poster abstract details

The radio continuum variations from galactic planetary nebulae in the process of the central star evolution without helium flashes are considered. On the base of our distance scale we obtained empirical evolutionary dependences for the ionized mass and the hydrogen atoms concentration. The parameters of theoretical model of the interacting stellar winds (ISW, Kwok 1982) are determined to reach an agreement between empirical and theoretical dependences. In this model the time dependences are obtained for for the critical frequency and the intrinsic flux density at several frequencies. The critical frequency is strongly depends on the mass of star nucleus. For the nucleus mass 0.546 $M_odot$ it is always lower than 1 GHz. But planetary nebula remains optically thick at 15 GHz up to kinematical age of 100 years if the central star mass is 0.836 M$_odot$. The intrinsic flux density changes in a wide interval of values in some orders of power. Radio flux at 15 GHz continues to increase up to age of $10^3$ years in model with 0.640 $M_odot$, up to $10^4$ years in the model with 0.565 $M_odot$. The maximum rate of the flux density 8$% yr^{-1}$ increase is obtained for the model with 0.640 $M_odot$ in the interval from 200 to 1100 years. Further the flux density decrease with rate 0.8 $% yr^{-1}$. We have obtained the sequences of instantaneous spectra at 0.960-21.7 GHz for a group of planetary nebulae (IC 418, NGC 6369 et al.) by using of RATAN-600. They were compared to theoretical conclusions.