  We use the three-dimensional Monte Carlo radiative transfer code HDUST to
model Be stars where the disc is tilted from the equatorial plane of the star.
We compute 128 models across 4 spectral types, B0, B2, B5 and B8, tilting the
disc by $0^o$, $10^o$, $20^o$, and $40^o$, while varying disc density according
to spectral type. We also compute every model for an average and high stellar
rotation rate. We first discuss non-tilted disc temperatures and show its
non-linear dependence on stellar and disc parameters. We find that tilting the
disc minimally affects the density-weighted average disc temperature, but
tilting does create a temperature asymmetry in disc cross sections, which is
more pronounced for a faster rotation rate. We also investigate the effect
tilting has on $V$-band magnitude, polarization, and the H$\alpha$ line.
Tilting the disc does affect these observables, but the changes are entirely
dependent on the position of the observer relative to the direction of tilt. We
find the observables that distinguish tilting from a change in density or
geometry are the H$\alpha$ line shape, where it can transition between
single-peaked and double-peaked, and the polarization position angle, whose
value is dependent on the projected major elongation axis of the disc on the
sky. We also present one early and one late-type model with warped discs. We
find their temperature structure varies a small amount from the uniformly
tilted models, and the different observables correspond to different tilt
angles, consistent with their expected volume of origin within the disc.

Solar and Stellar Astrophysics