  Asteroids of size larger than 0.15 km generally do not have periods P smaller
than about 2.2 hours, a limit known as cohesionless spin-barrier. This barrier
can be explained by means of the cohesionless rubble-pile structure model. In
this paper we will explore the possibility for the observed spin-barrier value
to be different for C and S-type Main Asteroids Belt (MBAs). On the basis of
the actual bulk density values, the expected ratio between the maximum rotation
periods is $P_C/P_S \approx 1.4 \pm 0.3$. Using the data available in the
asteroid LightCurve Data Base (LCDB) we have found that, as regards the mean
spin-barrier values and for asteroids in the 4-20 km range, there is a little
difference between the two asteroids population with a ratio $P_C/P_S \approx
1.20 \pm 0.04$. Uncertainties are still high, mainly because of the small
number of MBAs with known taxonomic class in the considered range. In the 4-10
km range, instead, the ratio between the spin-barriers seems closer to 1
because $P_C/P_S \approx 1.11 \pm 0.05$. This behavior could be a direct
consequence of a different cohesion strength for C and S-type asteroids of
which the ratio can be estimated.
