we have, even if it is in an approximate way. In Fig. 3 the evaporation rate $\Gamma_{\nu}$ is displayed for a hot rotating nucleus $^{160}$Yb. It becomes obvious that the deformation dependence of $\Gamma_{\nu}$ is essential and that assuming a deformation independent emission width could probably lead to wrong predictions.

The second approach we used so far to describe particle emission calculates the transition rates $\Gamma^{\mu\kappa}_\nu$ through the probability that a particle which impinges on the nuclear surface at a given point $\vec r_0\,'$ and with a given velocity $\vec v_0\,'$ is actually transmitted [@DPR95]. In this framework the quantity $\Gamma^{\mu\kappa}_\nu$ is determined as $$\Gamma^{\mu\kappa}_\nu = {d^2 n_\nu \over d\varepsilon_\mu d\ell_\kappa}  
                             \Delta\varepsilon \,\Delta \ell \; .
\label{eqtw10}$$

The number $n_\nu$ of particles of type $\nu$ which are emitted per time unit through the surface $S$ of the fissioning nucleus is given by $$n_\nu = \int\limits_S \! d\sigma \int \! d^3 p' \, f_\nu(\vec r_0\,', 
 \vec p\,') \, v'_\perp(\vec r_0\,') \, w_\nu( v'_\perp (\vec r_0\,'))$$ where the quantity $f_\nu(\vec r\,' , \vec p\,')$ corresponds to the quasi-classical phase-space distribution function [@DPR95].\
${}$\
${}$\
FIG. 4. Emission rates $\Gamma_n$ and $\Gamma_p$ for neutrons and protons obtained in the Weisskopf and the distribution 