SIMBAD references

To approach the galactic dynamo we solve the mean-field induction equation (with a 2D time-stepping code after Elstner et al. 1990, Geophys. Astrophys. Fluid Dyn. 38, 273) for a well-defined flow system. The turbulence pattern is assumed to be distributed in vertical direction (but to be uniform along the radius). It also extends to the galactic halo, where a fixed value of the rms velocity is defined. The mid-plane turbulence intensity is the free parameter in the theory. The turbulence electromotive force is computed without inclusion of the density stratification. The mean flow consists of the global galactic rotation and a vertical wind. The wind is increasing with the disk height. Uniform as well as spike-like radial profiles of the wind intensity are used. The dynamo is suppressed if intensive uniform winds are acting in the dynamo-active region. For winds separated from the dynamo domain there is generally a rather weak influence of the wind on the resulting field strength. The field geometry, however is drastically changed in the wind region. Weak vertical field components occur for horizontally uniform winds while rather strong vertical magnetic fields belong to a highly non-uniform (`spiky') wind profile.