  Context: We present 31.2 days of nearly continuous MOST photometry of the
roAp star 10Aql. 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 Bp = 0-5kG 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
(50.95microHz) is consistent with the main sequence nature of roAp stars. The
comparison with theoretical models yields a best fit for a 1.95Msun 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 (Prot>1 month) and
inclination (i>30\pm10deg.). 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.
