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We present results of a search for identification of modes responsible forthe six most significant frequency peaks detected in the rapidly rotating SPBstar $\mu$ Eridani. All published and some unpublished photometric data areused in our new analysis. The mode identification is carried out with themethod developed by Daszy\'nska-Daszkiewicz et al. employing the phases andamplitudes from multi-band photometric data and relying on the traditionalapproximation for the treatment of oscillations in rotating stars.  Models consistent with the observed mean parameters are considered. For thefive frequency peaks, the candidates for the identifications are searchedamongst unstable modes. In the case of the third frequency, which is an exactmultiple of the orbital frequency, this condition is relaxed. The systematicsearch is continued up to a harmonic degree $\ell =6$.  Determination of the angular numbers, $(\ell,m)$, is done simultaneously withthe rotation rate, $V_{\rm rot}$, and the inclination angle, $i$, constrainedby the spectroscopic data on the projected rotational velocity, $V_{\rmrot}\sin i$, which is assumed constant. All the peaks may be accounted for withg-modes of high radial orders and the degrees $\ell\le 6$. There aredifferences in some identifications between the models. For the twolowest--amplitude peaks the identifications are not unique. Nonetheless, theequatorial velocity is constrained to a narrow range of (135, 140) km/s.  Our work presents the first application of the photometric method of modeidentification in the framework of the traditional approximation and we believethat it opens a new promising direction in studies of SPB stars.

Oscillation modes in the rapidly rotating Slowly Pulsating B-type star $\bmu$ Eridani