Van de Hulst inversion

We first fit a polynomial expansion to each radial profile of white light intensity, i.e. polarized brightness (pB):

pB = A*(r)^-B + C*(r)^-D + F*(r)^-G

pB radial profile fits for August 17-20, 1996, West limb colatitude 265-275.

Note: LASCO data unavailable for August 19, so the fit is only to the Mauna Loa data.

We then use Van de Hulst inversion techniques to determine radial profiles of density From pB, since pB is proportional to the integral along the line of sight of electron density multiplied by a Thomson scattering function.

Ne = No*(a*(r)^-b + c*(r)^-d + f*(r)^-g)

No = 3.14e8 (Rsun/(G Msun mp) )

density AND temperature (calculated assuming radial hydrostatic equilibrium and the ideal gas law) radial profile fits for August 17-20, 1996, West limb colatitude 265-275.

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