Observed associations between the solar interior, corona, and solar wind

Using polarized brightness (pB) measurements made by the High Altitude Obse rvatory (HAO) Mauna Loa Mk III K-coronameter, we investigate the daily chan ges of path-integrated density at 1.15 R-circle dot. During 1996, when simu ltaneous pB and helioseismology data were available, we find that the corre lation of pB (at zero time lag and 20 degrees latitude lag) varies with lat itude in the same way that the subsurface differential rotation inferred fr om helioseismology does. The association is such that bands of higher pB co rrelation are associated with retrograde subsurface rotation and that lower pB correlation bands are associated with prograde subsurface rotation. We also show that polar coronal holes are distinguished by a nonrecurring long itudinal structure as opposed to a recurring structure in the quiet Sun. In addition, the levels of pB and standard deviation sigma(pB) of pB are abou t half of those of the neighboring quiet Sun. These statistical characteris tics of coronal density in polar holes and the quiet Sun were also present in 1993-1994 and are replicated in the statistics of the distant solar wind observed by Ulysses. The association of the density (pB) correlation with subsurface flow (when simultaneous data were available in 1996), together w ith the association of the latitudinal dependence of the statistical charac teristics (average, standard deviation, and autocorrelation function) of th e coronal (pB) and solar wind (Ulysses) density (when simultaneous data wer e available in 1993-1994), suggest a correlated variability of subsurface f low, coronal density, and solar wind density organized by solar latitude.