The calculated intermediate and high degree p-mode frequencies of stan
dard solar models show greater disagreement with the observations than
low degree modes. This leads to the conclusion that the subatmospheri
c structure of the models has to be improved. We are presenting solar
models with up-to-date input physics and controlled numerical accuracy
of 10(-5). For the outer boundary condition we use synthetic atmosphe
res fitted to the interior solution at tau approximate to 20. In addit
ion, a spatially variable mixing length parameter is employed to repro
duce the pressure-temperature stratification of the outer convective z
one calculated by 2D-hydrodynamical models we used for comparison. Wit
h this changed subatmospheric structure we could improve the agreement
between predicted and observed p-mode frequencies in our solar models
.