A method for the asteroseismic analysis of \beta Cephei stars is presented and applied to the star \nu Eridani .
The method is based on the analysis of rotational splittings , and their asymmetries using differentially-rotating asteroseismic models .
Models with masses around 7.13 { \mathrm { M } _ { \odot } } , and ages around 14.9 Myr , were found to fit better 10 of the 14 observed frequencies , which were identified as the fundamental radial mode and the three \ell = 1 triplets { g } _ { 1 } , { p } _ { 1 } , and { p } _ { 2 } .
The splittings and aymmetries found for these modes recover those provided in the literature , except for { p } _ { 2 } .
For this last mode , all its non-axysimmetric components are predicted by the models .
Moreover , opposite signs of the observed and predicted splitting asymmetries are found .
If identification is confirmed , this can be a very interesting source of information about the internal rotation profile , in particular in the outer regions of the star .

In general , the seismic models which include a description for shellular rotation yield slightly better results as compared with those given by uniformly-rotating models .
Furthermore , we show that asymmetries are quite dependent on the overshooting of the convective core , which make the present technique suitable for testing the theories describing the angular momentum redistribution and chemical mixing due to rotationally-induced turbulence .