Each file contains tabulated data for time-steady solar atmosphere
models that go from the "deep photosphere" (tau_Ross = 2) to the outer
heliosphere (1200 solar radii).  These models were published by
Cranmer et al. (2007), ApJ Suppl., 171, 520.

Column formats:

(1) height above photospheric base, in solar radii
(2) mass density, in g/cm^3
(3) solar wind outflow speed, in cm/s
(4) temperature (one-fluid average), in K
(5) radial magnetic field strength, in G
(6) Alfven wave amplitude, in cm/s

Files:

cvb07_pole.dat:  polar coronal hole at solar minimum
cvb07_equator.dat:  equatorial streamer at solar minimum
cvb07_active.dat:  active region open-flux model, with h = 0.07 Rsun.

For the polar coronal hole and equatorial streamer geometry, see
Figure 11.  The active region model received extra magnetic flux at
the base, specified by the "h" parameter (see equation 73).  The radial
magnetic fields used in the three models are shown in Figure 5.
The models have identical lower boundary conditions for the Alfven and
acoustic waves/turbulence.  The temperatures for all three models are
compared with one another in Figure 17.

(If you use these models for anything, there's probably no need to cite
this web page; just cite the Cranmer et al. (2007) paper.)

ADDENDUM (2010):

The file 'cvb07_theta28.dat' corresponds to the near-equatorial field
line that Hollweg et al. (2010, ApJ, 722, 1495) found best satisfied 
the Helios Faraday rotation fluctuation measurements.

ADDENDUM (2012):

I've also added a few other files corresponding to intermediate colatitudes.

NOTE: If one is using the Alfven wave amplitude to estimate nonthermal line
widths, one needs to divide the tabulated velocity by a factor of sqrt(2),
since the observed motions account for only HALF of the total wave energy
that exists in the plane transverse to the background magnetic field.