Uncertainties on the theoretical predictions for classical Cepheidpulsational quantities

摘要

Context. With their period-luminosity relation, “classical Cepheids” (CC) are the most common primary distance indicators withinthe Local Group, also providing an absolute calibration of important secondary distance indicators. However, the predicted positionof these pulsators in the HR diagram, along the so called blue loop, that is the expected distribution of Cepheids within the instabilitystrip is affected by several model inputs, reflecting upon the predicted PL relation.Aims. The aim of this work is to quantitatively evaluate the effects on the theoretical PL relation of current uncertainties on the chemicalabundances of Cepheids in the Large Magellanic Cloud (LMC) and on several physical assumptions adopted in the evolutionarymodels. We will separately analyse how the different factors influence the evolutionary and pulsational observables and the resultingPL relation.Methods. To achieve this goal we computed new sets of updated evolutionary and pulsational models.Results. As a result, we find that present uncertainties on the most relevant H and He burning reaction rates do not influence in arelevant way the loop extension in temperature. On the contrary, current uncertainties on the LMC chemical composition significantlyaffect the loop extension and also reflect in the morphology of the instability strip; however their influence on the predicted pulsationalparameters is negligible. We also discussed how overshooting and mass loss, sometimes suggested as possible solutions for thelong-standing problem of the Cepheid mass discrepancy, influence the ML relation and the pulsational parameters.Conclusions. In summary, the present uncertainties on the physical inputs adopted in the evolutionary codes and in the LMC chemicalcomposition are negligible for the prediction of the main pulsational properties. On the other hand, the inclusion of overshooting inthe previous hydrogen burning phase and/or of mass loss is expected to significantly change the resulting theoretical pulsational scenariofor Cepheids, as well as the calibration of their distance scale. These systematic effects are expected to influence the theoreticalCepheid calibration of the secondary distance indicators and in turn the resulting evaluation of the Hubble constant.