Speaker
Description
We present analytical and numerical models of linear radial pulsations in stellar structures with parameters representative of evolved stars in selected globular clusters. Motivated by recent observations of short-period, low-amplitude variables in NGC 3201 and NGC 6397, this work investigates whether linear adiabatic radial oscillations can reproduce the observed period ranges of these objects. Starting from the hydrodynamic equations of stellar structure, we formulate the radial oscillation problem under the assumption of small perturbations around hydrostatic equilibrium. The resulting equations are solved using Python-based numerical models of simplified stellar structures, scaled to physically plausible parameters that correspond to different evolutionary stages. The theoretical periods are then compared with observational samples reported in recent photometric studies. This comparison provides a physically grounded test of radial pulsation as a possible origin of the observed variability and clarifies the limits of this simplified interpretation.