  We present the first part of a spectroscopic and polarimetric study on a
sample of 58 Be stars that have been measured since 1998. The aim of the study
is to understand the timescales of disk variability, formation and dissipation
as a function of the properties (mass, luminosity and rotational velocity) of
the underlying B star. In this paper we classified the sample based on the
presence of emission or absorption of the H$\alpha$ line, and the shape of the
peak as single or double peak, as well as noting changes between emission and
non-emission states. We find a probability of $\sim 0.75$ percent per year that
an object in the sample will undergo such a change. We also present re-derived
values of the projected rotational velocities for the sample. When we compare
our polarization values with those from the literature, we find that most of
the stars do not show a change in the value of the polarization angle, however
a small number show significant changes which could be attributed to either
disk strength (optical depth) or geometry changes. Finally we show how, by
combining the (interstellar corrected) degree of polarization and the projected
rotational velocity, we can construct an inclination angle-free parameter that
includes the true equatorial velocity. Using this inclination angle-independent
parameter we show that the populations of single and double peak stars are
indistinguishable, giving further evidence that Be star line profiles are
essentially inclination angle driven.
