The circumgalactic medium ( CGM ) of nearby star-forming galaxies shows clear indications of \ion O6 absorption accompanied by little to no detectable \ion N5 absorption .
This unusual spectral signature , accompanied by highly non-uniform absorption from lower ionization state species , indicates that the CGM must be viewed as a dynamic , multiphase medium , such as occurs in the presence of turbulence .
Motivated by previous isotropic turbulent simulations , we carry out chemodynamical simulations of stratified media in a Navarro-Frenk-White ( NFW ) gravitational potential with a total mass of 10 ^ { 12 } M _ { \odot } and turbulence that decreases radially .
The simulations assume a metallicity of 0.3 Z _ { \odot } , a redshift zero metagalatic UV background , and they track ionizations , recombinations , and species-by-species radiative cooling using the MAIHEM package .
We compare a suite of ionic column densities with the COS-Halos sample of low-redshift star-forming galaxies .
Turbulence with an average one-dimensional velocity dispersion \approx 40 km s ^ { -1 } , corresponding to an energy injection rate of \approx 4 \times 10 ^ { 49 } erg yr ^ { -1 } , produces a CGM that matches many of the observed ionic column densities and ratios .
In this simulation , the N _ { N V } / N _ { O VI } ratio is suppressed from its equilibrium value due to a combination of radiative cooling and cooling from turbulent mixing .
This level of turbulence is consistent with expectations from observations of better constrained , higher-mass systems , and could be sustained by energy input from supernovae , gas inflows , and dynamical friction from dark matter subhalos .
We also conduct a higher resolution \approx 40 km s ^ { -1 } run which yields smaller-scale structures , but remains in agreement with observations .