An analytical model for a turbulent clumpy gas disk is presented where turbulence is maintained by the energy input due to supernovae .
Expressions for the disk parameters , global filling factors , molecular fractions , and star formation rates are given as functions of the Toomre parameter Q , the ratio between the cloud size and the turbulent driving length scale \delta , the mass accretion rate within the disk \dot { M } , the constant of molecule formation \alpha , the disk radius , the angular velocity , and its radial derivative .
Two different cases are investigated : a dominating stellar disk and a self-gravitating gas disk in z direction .
The turbulent driving wavelength is determined in a first approach by energy flux conservation , i.e .
the supernovae energy input is transported by turbulence to smaller scales where it is dissipated .
The results are compared to those of a fully gravitational model .
For Q = 1 and \delta = 1 both models are consistent with each other .
In a second approach the driving length scale is directly determined by the size of supernovae remnants .
Both models are applied to the Galaxy and can reproduce its integrated and local gas properties .
The influence of thermal and magnetic pressure on the disk structure is investigated .
We infer Q \sim 1 and \dot { M } \sim 0.05 - 0.1 M _ { \odot } yr ^ { -1 } for the Galaxy .