Testing global ISM models:: A detailed comparison of OVI column densities with fuse and copernicus data

We study the O VI distribution in space and time in a representative section of the Galactic disk using three-dimensional adaptive mesh refinement hydrodynamic and magnetohydrodynamic simulations of the interstellar medium ( ISM), including the disk-halo-disk circulation. The simulations describe a supernova-driven ISM on large (similar to 10 kpc) and small (similar to 1.25 pc) scales over a sufficiently large timescale (similar to 400 Myr) in order to establish a global dynamical equilibrium. The O vi column density, N( O VI), is monitored through line-of-sight measurements at different locations in the simulated disk. One has been deliberately chosen to be inside of a hot bubble, like our own Local Bubble, while the other locations are random. We obtain a correlation between N( O VI) and distance, which is independent of the observer's vantage point in the disk. In particular, the location of the observer inside a hot bubble does not have any influence on the correlation, because the contribution of an individual bubble ( with a typical extension of 100 pc) is negligibly small. We find a remarkable agreement between the O VI column densities ( as a function of distance) and the averaged O VI density (similar to 1.8 x 10(-8) cm(-3)) in the disk from our simulations and from the values observed with Copernicus and FUSE. Our results strongly support the important role of turbulent mixing in the distribution of O VI clumps in the ISM. Supernova-induced turbulence is quite strong and unavoidable due to shearing motions in the ISM, and it operates on a large range of scales.