Spherical convective dynamo with 5 times solar rotation:
The rotation in the reference frame is Omega0=1.35000e-05 1/s
The azimuthal velocity gives the difference reference frame, so 
positive values = faster rotation than the reference frame and vice versa.

The magnetic field shows clear cyles with a frequency of around 2.6 years.
The time resolution is around 13.8 days and the whole data set spanns 
around 37.8 years

For numerical reasons, we have to leave out the poles, so we cut the last 
15 degrees. The simulation spans from 0.7 to 1.0 in radius, but the density 
stratification is not realistic.

Please find the overview of the quantites contained in the fit files:

nr:      number of radial grid points
ntheta:  number of latitudinal grid points
ntime :  number of points in time
ncomp :  components, with radial, latitudinal, azimuthal direction

File                     structure                 units

magnetic_field     [nr,ntheta,ntime,ncomp]         Gauss

velocity_field     [nr,ntheta,ntime,ncomp]          m/s

sound_speed        [nr,ntheta,ntime]                m/s

density            [nr,ntheta,ntime]                kg/m3

time               [ntime]                          s

radius             [nr]                             m

theta              [ntheta]                         rad 
(Colatitude: theta=0 -> north pole)


More information about these models can be found in:

Warnecke, J. and Kapyla, M. J.,: 2020, Rotational dependence of turbulent 
  transport coefficients in global convective dynamo simulations of 
  solar-like stars, Astron. Astrophys., accepted, arXiv: 1910.06776

Warnecke, J.: 2018, Dynamo cycles in global convection simulations of 
  solar-like stars, Astron. Astrophys., 616, A72

Kapyla, P. J., Mantere, M. J., Cole, E., Warnecke, J., & Brandenburg, A.: 
  2013, Effects of strong stratification on equatorward dynamo wave 
  propagation, Astrophys. J., 778, 41.