  We present a new method for determining the location of active bands of
latitude on solar-type stars, which uses stellar-cycle-induced frequency shifts
of detectable solar-like oscillations. When near-surface activity is
distributed in a non-homogeneous manner, oscillation modes of different angular
degree and azimuthal order will have their frequencies shifted by different
amounts. We use this simple concept, coupled to a model for the spatial
distribution of the near-surface activity, to develop two methods that use the
frequency shifts to infer minimum and maximum latitudes for the active bands.
Our methods respond to the range in latitude over which there is significant
magnetic flux present, over and above weak basal ephemeral flux levels. We
verify that we are able to draw accurate inferences in the solar case, using
Sun-as-a-star helioseismic data and artificial data. We then apply our methods
to Kepler data on the solar analogue HD173701, and find that its active bands
straddle a much wider range in latitude than do the bands on the Sun.
