Format of WSA output file
WSA uses grids on the surface of a sphere. The grid is evenly spaced in both theta and phi.
The numerical grid has N points evenly spaced in latitude.
The numerical grid has M points evenly spaced in the azimuthal direction.

For 2.5 degree resolution N=144, M=72          - typically used for NSO data
For 5 degree resolution N=72, M=36             - typically used for MWO data

The output file from the WSA model has the following format.

 Line 1:  CR number and latest longitude
 B1AU   - an array of size (N,M+1) formatted with 12 records per line
 RAT    - an array of size (N,M+1) formatted with 12 records per line
 TT     - an array of size (N,M+1) formatted with 12 records per line
 PP     - an array of size (N,M+1) formatted with 12 records per line
 BPARP  - an array of size (N,M) formatted with 12 records per line
 PP_ecl - a vector of size (N) formatted with 12 records per line
 TT_ecl - a vector of size (N) formatted with 12 records per line
 PP_ss  - a vector of size (N) formatted with 12 records per line
 TT_ss  - a vector of size (N) formatted with 12 records per line
 Line EOF-3 : the location of the models outer radius in units of solar radius
 Line EOF-2 : the order of spherical harmonics retained in the magnetogram fit
 Line EOF-1 : a bookkeeping entry - if NSO appears then source is Kitt Peak, if MWO then
              source is Mount Wilson

For 2.5 degree resolution N=144, M=72          - typically used for NSO data
For 5 degree resolution N=72, M=36


Nick Arge provided the following text to describe the output in these files for the case of 5 degree resolution. Normally we run at 2.5 degree resolution. This produces files with 4420 lines. If there are fewer lines then the output is for a 5 degree resolution case.

--------------------------------------------------------------------------------------


!----------------------------
! Size of 5 degree grid
!----------------------------
integer, PARAMETER :: MPHI_s = 72
integer, PARAMETER :: MTHE_s = 36

integer, PARAMETER  ::  MTHEP_s = MTHE_s+1


REAL   ::   B1AU(MPHI_s,MTHEP_s)
REAL   ::   RAT(MPHI_s,MTHEP_s)
REAL   ::   TT(MPHI_s,MTHEP_s)
REAL   ::   PP(MPHI_s,MTHEP_s)
REAL   ::   BPARP(MPHI_s,MTHE_s)
REAL   ::   PP_ecl(MPHI_s), TT_ecl(MPHI_s)

 2000    FORMAT (2(1x,I5))
 3000    FORMAT (12(F10.3,1X))
 4000    FORMAT (12(F10.4,1X))
 5000    FORMAT (12(F10.5,1x))
 5500    FORMAT (12(ES15.5,1x))  ! Scientific notation  field 15 spaces wide,
                                                  ! places after decimal
        
         !---------------------------------------------------
         ! Carrington Rotation, Longitude of left edge of map
         !---------------------------------------------------                    
         WRITE (26,2000) NCARR, NCARRLONG

         !---------------------------------------------------------------------------------
         ! The index i corresponds to every 5 deg of longitude
         ! (i.e., 2.5 deg, 7.5 deg, ..., 357.5 deg) at the source surface. 
         ! The index j corresponds to every 5 deg
         ! of latitude (i.e., -87.5 deg, -82.5 deg, ..., +87.5 deg) on the grid
         !
         ! The MTHEP_s j corresponds to the MPHI_s values (72 values for a 5 degree
         ! grid) of a given parameter (e.g.,
         ! source surface field strength, expansion factor) calculated at the ecliptic.
         !
         ! ******* Note, the program was originally written ASSUMING that the maps are
         !               STANDARD CARRINGTON maps (i.e., left edge corresponds to 0 deg
         !               longitude and right edge 360 deg). According, all longitudes given
         !               below need to be adjusted by the NCARRLONG value provided above.
         !-----------------------------------------------------------------------------------

         !-----------------------------------------------------------------------------

         !--------------------------------------------
         ! new Sept 30, 2003 - changed format
         ! B1AU is source-surface field in nano-Tesla
         !--------------------------------------------
         WRITE (26,5500) ((B1AU(I,J), I=1,MPHI_s), J=1,MTHEP_s)


         !-------------------------------------------------------------------
         ! RAT is flux-tube expansion factor evaluated at the source surface
         !-------------------------------------------------------------------
         WRITE (26,3000) ((MAX(MIN(RAT(I,J),99999.),-9999.),I=1,MPHI_s), &
                           J=1,MTHEP_s)

         !-------------------------------------------------------------------
         ! TT is theta (co-latitude in radians) of the photospheric footpoint
         ! coordinates of the source-surface (i.e., open) field lines.
         !-------------------------------------------------------------------
         WRITE (26,4000) ((MAX(MIN(TT(I,J),9999.),-999.),I=1,MPHI_s), &
                           J=1,MTHEP_s)

         !-----------------------------------------------------------------------------
         ! PP is phi (longitude in radians) of the photospheric footpoint
         ! coordinates of the source-surface (i.e., open) field lines.
         ! Remember that the value
         ! of NCARRLONG needs to be added to these numbers (after they have been
         ! converted into degrees).
         !
         ! The SIGN of these numbers indicate the POLARITY of the magnetic field lines
         ! + = directed away from Sun
         ! - = directed inward
         !------------------------------------------------------------------------------
         WRITE (26,4000) ((MAX(MIN(PP(I,J),9999.),-999.),I=1,MPHI_s), &
                           J=1,MTHEP_s)

         !----------------------------------------------------------
         ! BPARP is the photospheric field in Gauss for every 5 deg
         ! of longitude and latitude at the photosphere.
         !----------------------------------------------------------
         WRITE (26,5000) ((MAX(MIN(BPARP(I,J),999.),-999.),I=1,MPHI_s), &
                           J=1,MTHE_s)

         !-----------------------------------------------------------------------------
         ! PP_ecl are the longitudinal values (in radians) of ecliptic (sub-earth point)
         !------------------------------------------------------------------------------
         WRITE (26,4000) (MAX(MIN(PP_ecl(I),9999.),-999.),I=1,MPHI_s)

         !-----------------------------------------------------------------
         ! TT_ecl is co-latitude (in radians) of ecliptic (sub-earth point)
         !------------------------------------------------------------------
         WRITE (26,4000) (MAX(MIN(TT_ecl(I),9999.),-999.),I=1,MPHI_s)


         !----------------------------------------------------------
         ! NM is the number of spherical harmonics for the L number
         !----------------------------------------------------------

         ! new feb 18, 2003 -------------------------------------------
         WRITE (26,'(a17,1x,f6.2)') 'outer radius = ',outer_rad
         WRITE (26,'(a5,1x,i3)') 'NM = ',NM
         !--------------------------------------------------------------