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Context. Asteroseismic determinations of structural parameters of hot Bsubdwarfs (sdB) have been carried out for more than a decade now. Theseanalyses rely on stellar models whose reliability for the required task needsto be evaluated critically. Aims. We present new models of the so-called thirdgeneration (3G) dedicated to the asteroseismology of sdB stars. Theseparameterized models are complete static structures suitable for analyzing bothp- and g-mode pulsators, contrary to the former second generation (2G) modelsthat were limited to p-modes. While the reliability of the 2G models has beensuccessfully verified in the past, this important test still has to beconducted on the 3G structures. Methods. The close eclipsing binary PG 1336-018provides a unique opportunity to test the reliability of sdB models. Wecompared the structural parameters of the sdB component in PG 1336-018 obtainedfrom asteroseismology based on the 3G models, with those derived independentlyfrom the modeling of the reflection/irradiation effect and the eclipsesobserved in the light curve. Results. The stellar parameters inferred fromasteroseismology using the 3G models are found to be remarkably consistent withboth the preferred orbital solution obtained from the binary light curvemodeling and the updated spectroscopic estimates for the surface gravity of thestar. We also show that the uncertainties on the input physics included instellar models have no noticeable impact, at the current level of accuracy, onthe structural parameters derived by asteroseismology. Conclusions. The stellarmodels presently used to carry out quantitative seismic analyses of sdB starsare reliable for the task. The stellar parameters inferred by this technique,at least for those that could be tested (M*, R*, and log g), appear to be bothvery precise and accurate, as no significant systematic effect has been found.

Third generation stellar models for asteroseismology of hot B subdwarf stars. A test of accuracy with the pulsating eclipsing binary PG 1336--018