Characterising the turbulent multiphase halos with periodic box
  simulations
  Turbulence in the intracluster medium (ICM) is driven by active galactic
nuclei (AGNs) jets, by mergers, and in the wakes of infalling galaxies. It not
only governs gas motion but also plays a key role in the ICM thermodynamics.
Turbulence can help seed thermal instability by generating density
fluctuations, and mix the hot and cold phases together to produce intermediate
temperature gas ($10^4$--$10^7$ $\mathrm{K}$) with short cooling times. We
conduct high resolution ($384^3$--$768^3$ resolution elements) idealised
simulations of the multiphase ICM and study the effects of turbulence strength,
characterised by $f_{\mathrm{turb}}$ ($0.001$--$1.0$), the ratio of turbulent
forcing power to the net radiative cooling rate. We analyse density and
temperature distribution, amplitude and nature of gas perturbations, and
probability of transitions across the temperature phases. We also study the
effects of mass and volume-weighted thermal heating and weak ICM magnetic
fields. For low $f_{\mathrm{turb}}$, the gas is distribution is bimodal between
the hot and cold phases. The mixing between different phases becomes more
efficient with increasing $f_{\mathrm{turb}}$, producing larger amounts of the
intermediate temperature gas. Strong turbulence ($f_{\mathrm{turb}}\geq0.5$)
generates larger density fluctuations and faster cooling, The rms logarithmic
pressure fluctuation scaling with Mach number
$\sigma_{\ln{\bar{P}}}^2\approx\ln(1+b^2\gamma^2\mathcal{M}^4)$ is unaffected
by thermal instability and is the same as in hydro turbulence. In contrast, the
density fluctuations characterised by $\sigma_s^2$ are much larger, especially
for $\mathcal{M}\lesssim0.5$. In magnetohydrodynamic runs, magnetic fields
provide significant pressure support in the cold phase but do not have any
strong effects on the diffuse gas distribution, and nature and amplitude of
fluctuations.
