If rotational splitting of modes with can be measured, then the interior distribution of angular velocity can be estimated by techniques such as those described in section 2.3.1. Gough and Kosovichev (1993) present an inversion for the solar interior rotation for a case where the standard errors on the frequencies are Hz. Such high precision will not normally be attained in the observing schedule available to STARS, so such detailed inversions could be achieved only for more rapidly rotating stars, since acceptable data errors scale linearly with . What can be achieved, however, are broad averages throughout the stellar interior, the most accurate being weighted essentially by the reciprocal of the sound speed and having a relative error of order , where T is the duration of the observation. Coupled with activity data indicating rotation rate of the surface, information about radial shear can thereby be obtained. Were one able to distinguish a difference in splittings between the and 2 modes, this would give some broad indication of latitudinal variation of rotation in the stellar interior.