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Meeting Update

Initial magnetic field is a dipole outside that transitions to a uniform Z field inside of a sphere of radius R/2. No details of smoothing distance in paper.
Initial density field is uniform in side a sphere - and is parker wind solution outside
Velocity is zero inside sphere and parker wind solution outside
Pressure is isothermal outside (from parker wind), and hydrostatic inside.
- Note they calculate P from radial momentum equation, isothermal EOS, and solution for parker wind velocity. I calculate radial velocity and use density equation to get rho, and isothermal EOS to get pressure.
Density is constant inside and parker solution outside.
Gravity is GM/R^{2 outside, and uniform sphere gravity inside. Note that M used for outside gravity does not equal 4/3 pi r}3^{rho inside}
Density, velocity, and pressure are stepped on inside of r=1.5 R (however, we cannot do this without analytic solution for non-isotropic parker wind).
Magnetic field is free to evolve inside and outside.
They discuss 4 layer model of Matt and Pudritz
1. v_poloidal parallel to B_poloidal
2. rho and P held constant
3. v set to zero ( v_phi is corotating)
4. B_poloidal held constant and B_phi is extrapolated inward to not have any poloidal current (curl of B_phi = 0)
- Each of these layers is approximately only 1 zone thick (the surface of the star is 30 zones in radius)

The development branch of the code now supports parallel HDF5.
On bluehive need to use astrobear/b3 module
Need to add -D_PHDF5 to CPPFLAGS in Makefile.inc
Set lParallelHDF5=.true. in GlobalData namelist.
Haven't tested this on BGQ.
If restarting from older files, need to open and rewrite chombo files without lParallelHDF5=.true.
There is a lReOutput flag that can be set along with lPostProcess to output the HDF5 files in a format compatible with ParallelHDF5=.true. restarts.