  As is well known, pulsars are extremely stable rotators. However, although
slowly, they spin down thanks to brake mechanisms, which are in fact still
subject of intense investigation in the literature. Since pulsars are usually
modelled as highly magnetized neutron stars that emit beams of electromagnetic
radiation out of their magnetic poles, it is reasonable to consider that the
spindown has to do with a magnetic brake. Although an interesting and simple
idea, a pure magnetic brake is not able to adequately account for the spindown
rate. Thus, many alternative spindown mechanisms appear in the literature,
among them the pulsar wind model, where a wind of particles coming from the
pulsar itself can carry part of its rotational kinetic energy. Such a spindown
mechanism depends critically on three parameters, namely, the dipole magnetic
field $B$, the angle between the magnetic and rotation axes $(\phi)$, and the
density of primary particles $(\zeta)$ of the pulsar's magnetosphere.
Differently from a series of articles in this subject, we consider for the
first time in the literature a statistical modelling which includes a
combination of a dipole magnetic and wind brakes. As a result, we are able to
constrain the above referred parameters in particular for Crab and Vela
pulsars.
