The files accessible from the table below are heliographic maps centered on the event times according to the SHINE campaign. The magnetic fields are from Fe I 525.2 nm and have been corrected for the saturation effects. The heliographic maps have been computed using the Shrauner-Scherrer method to resolve the zonal and meridional components. Each point was tracked according to its local rotation rate for the vector component resolution then plotted according to its heliographic longitude at the time of the central meridian passage.

A paper giving a description of our coordinate transformation methods has been submitted to Solar Physics.

The files currently linked were revised 18-Feb-2005 to correct an error in the averaging process whereby the effects of differential rotation were applied twice in the previous set of results. The error smeared small features but did not alter the basic magnetic configuration over the solar surface. The current files should be used in place of the previous files although the modifications are small.

The following table points to heliographic maps created in the same was as above but using for input magnetic fields measured using two spectroscopic samples near the core of the NaD1 line.

The image below illustrates the photospheric context of the magnetograms based on the two line pairs used above. The Fe I line at 5250 Angstroms has traditionally been used by the MWO project while the magnetograms based on the Na D1 core are a recent addition to the set of reduced data from this project. Due to the height of formation for this spectral sample, some of the non-potential properties of the magnetic field in the lower photosphere are mitigated and this set of magnetograms may provide a more appropriate set of boundary conditions for the calculation of the source surface magnetic field.