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Besides their own intrinsic interest, correct interpretation of solar surfacemagnetic field observations is crucial to our ability to describe the globalmagnetic structure of the solar atmosphere. Photospheric magnetograms are oftenused as lower boundary conditions in models of the corona, but not data fromthe nearly force-free chromosphere. National Solar Observatory's (NSO) SynopticOptical Long-term Investigations of the Sun VSM (Vector Spectromagnetograph)produces full-disk line-of-sight magnetic flux images deriving from bothphotospheric and chromospheric layers on a daily basis. In this paper, weinvestigate key properties of the magnetic field in these two layers using morethan five years of VSM data. We find from near-equatorial measurements that theeast-west inclination angle of most photospheric fields is less than about12{\deg}, while chromospheric fields expand in all directions to a significantdegree. Using a simple stereoscopic inversion, we find evidence thatphotospheric polar fields are also nearly radial but that during 2008 thechromospheric field in the south pole was expanding superradially. We obtain aspatially resolved polar photospheric flux distribution up to 80{\deg} latitudewhose strength increases poleward approximately as cosine(colatitude) to thepower 9-10. This distribution would give a polar field strength of 5-6 G. Webriefly discuss implications for future synoptic map construction and modeling.

A Comparative Study of Magnetic Fields in the Solar Photosphere and Chromosphere at Equatorial and Polar Latitudes