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 All published and some unpublished photometric data are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