  Oscillation mode frequencies of stars are typically treated as static for a
given stellar model. However, in reality they can be perturbed by time varying
sources such as magnetic fields and flows. We calculate the sensitivities of
radial p-mode oscillations of a set of models for masses between 0.7-3.0
M$_{\odot}$ from the main sequence to the early asymptotic giant branch. We fit
these mode sensitivities with polynomials in fundamental stellar parameters for
six stages of stellar evolution. We find that the best-fitting relations differ
from those proposed in the literature and change between stages of stellar
evolution. Together with a measure of the strength of the perturbation, e.g.,
of the level of magnetic activity, the presented relations can be used for
assessing whether a star's observed oscillation frequencies are likely to be
close to the unperturbed ground state or whether they should be adjusted.
