Context : There are numerous examples of accretion discs in binary systems where the disc midplane is believed to be inclined relative to the binary orbit plane .

Aims : We aim to examine the detailed disc structure that arises in a misaligned binary system as a function of the disc aspect ratio h , viscosity parameter \alpha , disc outer radius R , and binary inclination angle \gamma _ { F } .
We also aim to examine the conditions that lead to an inclined disc being disrupted by strong differential precession .

Methods : We use a grid-based hydrodynamic code to perform 3D simulations .
This code has a relatively low numerical viscosity compared with the SPH schemes that have been used previously to study inclined discs .
This allows the influence of viscosity on the disc evolution to be tightly controlled .

Results : We find that for thick discs ( h = 0.05 ) with low \alpha , efficient warp communication in the discs allows them to precess as rigid bodies with very little warping or twisting .
Such discs are observed to align with the binary orbit plane on the viscous evolution time .
Thinner discs with higher viscosity , in which warp communication is less efficient , develop significant twists before achieving a state of rigid-body precession .
Under the most extreme conditions we consider ( h = 0.01 , \alpha = 5 \times 10 ^ { -3 } and \alpha = 0.1 ) , we find that discs can become broken or disrupted by strong differential precession .
Discs that become highly twisted are observed to align with the binary orbit plane on timescales much shorter than the viscous timescale , possibly on the precession time .

Conclusions : We find agreement with previous studies that show that thick discs with low viscosity experience mild warping and precess rigidly .
We also find that as h is decreased substantially , discs may be disrupted by strong differential precession , but for disc thicknesses that are significantly less ( h = 0.01 ) than those found in previous studies ( h = 0.03 ) .