  Context. Asteroseismic determinations of structural parameters of hot B
subdwarfs (sdB) have been carried out for more than a decade now. These
analyses rely on stellar models whose reliability for the required task needs
to be evaluated critically. Aims. We present new models of the so-called third
generation (3G) dedicated to the asteroseismology of sdB stars. These
parameterized models are complete static structures suitable for analyzing both
p- and g-mode pulsators, contrary to the former second generation (2G) models
that were limited to p-modes. While the reliability of the 2G models has been
successfully verified in the past, this important test still has to be
conducted on the 3G structures. Methods. The close eclipsing binary PG 1336-018
provides a unique opportunity to test the reliability of sdB models. We
compared the structural parameters of the sdB component in PG 1336-018 obtained
from asteroseismology based on the 3G models, with those derived independently
from the modeling of the reflection/irradiation effect and the eclipses
observed in the light curve. Results. The stellar parameters inferred from
asteroseismology using the 3G models are found to be remarkably consistent with
both the preferred orbital solution obtained from the binary light curve
modeling and the updated spectroscopic estimates for the surface gravity of the
star. We also show that the uncertainties on the input physics included in
stellar models have no noticeable impact, at the current level of accuracy, on
the structural parameters derived by asteroseismology. Conclusions. The stellar
models presently used to carry out quantitative seismic analyses of sdB stars
are 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 both
very precise and accurate, as no significant systematic effect has been found.
