Scaling relations for the turbulent, non-self-gravitating, neutral component of the interstellar medium

Scaling relations for the turbulent, non-self-gravitating, neutral component of the interstellar medium (ISM) are derived on the basis of von Weizsacker's phenomenological model of compressible turbulence. The turbulent velocity upsilon, column density N, gas density rho, and mass M scale with region size I as upsilon similar to N similar to rho(-1) similar to M(1/5) similar to l(1/2). In addition, the spectral energy function E(k) similar to k(-2) for wavenumber k, and the diffuse cloud mass spectrum N(M) similar to M(-2). These derived relations are shown to be in good agreement with observations. The scaling of magnetic field strength in these regions is briefly discussed, but uncertainties involved with compressible MHD turbulence preclude any definite predictions. It appears that turbulent hydrodynamics is the common underlying physics which controls many of the properties of the neutral component of the ISM, independent of self-gravity.