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Faraday rotation measures (RMs) of the polarized emission from extragalacticradio sources occulted by the coronal plasma were used to infer the radialprofile of the inner heliospheric magnetic field near solar minimum activity.By inverting LASCO/SOHO polarized brightness (pB) data taken during the days ofobservations on May 1997, we retrieved the electron density distribution alongthe lines of sight to the sources, thus allowing to disentangle the two plasmaproperties that contribute to the observed RMs. By comparing the observed RMvalues to those theoretically predicted by a power-law model of the radialcomponent of the coronal magnetic field, using a best-fitting procedure, wefound that the radial component of the inner heliospheric magnetic field can benicely approximated by a power-law of the form B_r = 3.76 r^{-2.29} G in arange of heights from about 5 to 14 solar radii. Finally, our analysis suggeststhat the radial computation of the potential field source surface (PFSS) modelfrom the Wilcox Solar Observatory (WSO), assuming a radial field in thephotosphere and a source surface located at R_{ss} = 2.5 solar radii, is thepreferred choice near solar minimum.

The radial profile of the inner heliospheric magnetic field as deduced from Faraday rotation observations