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We use the three-dimensional Monte Carlo radiative transfer code HDUST tomodel 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 thedisc by $0^o$, $10^o$, $20^o$, and $40^o$, while varying disc density accordingto spectral type. We also compute every model for an average and high stellarrotation rate. We first discuss non-tilted disc temperatures and show itsnon-linear dependence on stellar and disc parameters. We find that tilting thedisc minimally affects the density-weighted average disc temperature, buttilting does create a temperature asymmetry in disc cross sections, which ismore pronounced for a faster rotation rate. We also investigate the effecttilting has on $V$-band magnitude, polarization, and the H$\alpha$ line.Tilting the disc does affect these observables, but the changes are entirelydependent on the position of the observer relative to the direction of tilt. Wefind the observables that distinguish tilting from a change in density orgeometry are the H$\alpha$ line shape, where it can transition betweensingle-peaked and double-peaked, and the polarization position angle, whosevalue is dependent on the projected major elongation axis of the disc on thesky. We also present one early and one late-type model with warped discs. Wefind their temperature structure varies a small amount from the uniformlytilted models, and the different observables correspond to different tiltangles, consistent with their expected volume of origin within the disc.

Non-LTE Monte Carlo Radiative Transfer. III. The thermal properties of Tilted and Warped Be Star Discs