- Bd-synoptic - results of magnetic field reconstruction from a current daily full-disk magnetogram of the visible side, and from the reconstructed magnetic field of the last synoptic map on the far side of the Sun.
- Synoptic - ðresults of the magnetic field reconstruction from the last
synoptic magnetogram (the method of reconstruction from the Bl-component [Hoeksema, J.T.: 1984, Structure and
Evolution of The Large Scale Solar and Heliospheric Magnetic Fields,
*Ph. D. Diss*., Stahford Univ..])

__*r.fits__- files with data on the Br-component for a current day or for the last synoptic map. The data are written as the Br(i,j), set corresponding to a grid at steps of 1 heliogeographic degree in the ranges f - [0^{0}, 359^{0}] and q - [-90^{0},90^{0}]. These files are, in principle, sufficient for obtaining all other results if we make use of a classical scheme for magnetic field reconstruction from the radial component (The Neuman problem).__*.WGZ__- packed weight *.WGT file. Contains harmonic expansion coefficients of the magnetic potential corresponding to the *r.fits data. The files with the *.WGT expansion are the solution of the Neuman problem for corresponding *r.fits files, and make it possible to calculate a total magnetic field vector at any point of space. The number of terms of the harmonic expansion corresponds to the main index Nmax=90. files, and programs for calculating the magnetic field in the FORTRAN and IDL languages are attached in the Programs section.__*rs.fits__- fits files with data on the Br-component for a current day and for the last synoptic map. These data are the result of an averaging of the *r.fits data over spherical areas 10^{0}in size. The grid of recording is at steps of 2^{0}. The averaged data reproduce the medium-scale magnetic structure, and can be compared with Wilcox Solar Observatory measurements.__*ls.fits__- fits files with data on the Bl-component for a current day or for the last synoptic rotation. It is calculated from the *S.WGT files. The grid is at steps of 2^{0}.__*S.WGZ__- packed weight *.WGT file. Contains harmonic expansion coefficients of the magnetic potential corresponding to the *rs.fits data. The number of harmonic expansion terms corresponds to the main index Nmax=30.__*SC.WGZ__- packed weight *.WGT file. Contains harmonic expansion coefficients of the magnetic potential obtained by using a "radial-2.5" correction of the boundary Bl field (*ls.fits). The number of harmonic expansion terms corresponds to the main index Nmax=30.__*SCC.WGZ__- packed weight *.WGT file. Contains harmonic expansion coefficients of the magnetic potential obtained by using a "radial-3.25" correction of the boundary Bl field (*ls.fits). The number of harmonic expansion terms corresponds to the main index Nmax=30.__*rws.fits__- fits files with data on the Br-component for a current day or for the last synoptic map on the source surface. They are calculated from the *S.WGT file. The grid is at steps of 2^{0}.__*rwsc.fits__- fits files with data on the Br-component for a current day or for the last synoptic map on the source surface. They are calculated from the *SC.WGT file. The grid is at steps of 2^{0}.__*rwscc.fits__- fits files with data on the Br-component for a current day or for the last synoptic map on the source surface. They are calculated from the *SCC.WGT file. The grid is at steps of 2^{0}.

The Holes ñsection contains a current calculation of regions
of open field lines, and of their physical characteristics, based on data such as Bd-synoptic.
The field lines are calculated from uniformly distributed (at steps of 4^{0})
on the source surface) start point. Their bases are shown in different colors for different
open regions. The designations are:

- Ss - area of the open region on the source surface.
- Sp - area of the open region at the photosphere.
- Sstot - total area of the source surface [4p*(2.5R
_{Sol})^{2}]. - Sptot - total area of the photosphere (4p*R
^{2}_{Sol}). - E - energy of the open magnetic field region.
- Etot - total energy of the closed and open magnetic field. This quantity is relatively arbitrary as it depends on the smallest scales of the magnetic field. With an increase in resolution of the boundary field, a total energy will have a larger value.
- Eopen - energy of the entire open magnetic field.
- F - magnetic field flux of the open region passing through an area of the source surface.
- F
^{(+)}_{tot }and F^{(-)}_{tot}- total positive and negative magnetic field fluxes crossing the source surface.

The system generates new data, and updates current images (except for __Holes__)
about every 2-3 hours after the appearance of a new daily magnetogram in the Kitt Peak catalog.
A further about 8 hours are required for updating __Holes__.

Currently the proposed version should be regarded as a preliminary one. Information that
is generated by the system at this stage requires a still greater comparative analysis before
any conclusive inference is made concerning the degree of its correspondence to the present
physical picture of the dynamics of the solar magnetic structure. It is not yet fully clear
how substantial would be the underlying approximations associated with the uncertainty of data
for the far side in the main. Without such an analysis, however, we can be confident in the
correctness of calculations spanning the heights on the order of the solar radius above the
visible side of the disk. These issues were discussed at length in a paper of G.V. Rudenko: 2001,
*Solar Phys*, **198**, 5. A further analysis and comparison of results will,
perhaps, choose a corrective addition that is appropriate for the boundary conditions for the
Bd-component used here. I will greatly appreciate having any information that would be useful
for a further development of this system. With all questions concerning the operation of the
system please apply to George Rudenko.