Context : We present 31.2 days of nearly continuous MOST photometry of the roAp star 10 Aql .

Aims : The goal was to provide an unambiguous frequency identification for this little studied star , as well as to discuss the detected frequencies in the context of magnetic models and analyze the influence of the magnetic field on the pulsation .

Methods : Using traditional Fourier analysis techniques on three independent data reductions , intrinsic frequencies for the star are identified .
Theoretical non-adiabatic axisymmetric modes influenced by a magnetic field having polar field strengths B _ { \mathrm { P } } = 0–5 kG were computed to compare the observations to theory .

Results : The high–precision data allow us to identify three definite intrinsic pulsation frequencies and two other candidate frequencies with low S/N .
Considering the observed spacings , only one ( 50.95 \mu Hz ) is consistent with the main sequence nature of roAp stars .
The comparison with theoretical models yields a best fit for a 1.95 M _ { \sun } model having solar metallicity , suppressed envelope convection , and homogenous helium abundance .
Furthermore , our analysis confirms the suspected slow rotation of the star and sets new lower limits to the rotation period ( P _ { rot } \geq 1 month ) and inclination ( i > 30 \pm 10 ^ { \circ } ) .

Conclusions : The observed frequency spectrum is not rich enough to unambiguously identify a model .
On the other hand , the models hardly represent roAp stars in detail due to the approximations needed to describe the interactions of the magnetic field with stellar structure and pulsation .
Consequently , errors in the model frequencies needed for the fitting procedure can only be estimated .
Nevertheless , it is encouraging that models which suppress convection and include solar metallicity , in agreement with current concepts of roAp stars , fit the observations best .