  Close binaries ($a_{bin} < 20$ au) are known to harbor planets, yet planet
formation is unlikely to succeed in such systems. Studying the dynamics of
disks in close binaries can help to understand how those planets could have
formed. We study the impact that numerical and physical parameters have on the
dynamics of disks in close binaries. We use the $\gamma$-Cephei system as an
example and focus on disk quantities such as disk eccentricity and the
precession rate as indicators for the dynamical state of the disks. We simulate
disks in close binaries by performing two-dimensional radiative hydrodynamical
simulations using a modified version of the Fargo code. First, we perform a
parameter study for different numerical parameters to confirm that our results
are robust. In the second part, we study the effects of different masses and
different viscosities on the disks' dynamics. Previous studies on radiative
disks in close binaries used too low resolutions and too small simulation
domains, which impacted the disk's dynamics. We find that radiative disks in
close binaries, after an initialization phase, become eccentric with mean
eccentricities between 0.06 to 0.27 and display a slow retrograde precession
with periods ranging from $4 - 40T_{bin}$ which depends quadratically on the
disk's mean aspect ratio. In general, the disks show a coherent, rigid
precession which can be broken, however, by changes in the opacity law reducing
the overall eccentricity of the disk.
