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To explore the difference between the most two recent solar minima, weanalyze the in-situ ACE and ULYSSES observations and examine the distributionsof the three types of solar wind (streamer-stalk-associated wind, wind fromoutside the streamer stalk that can be associated, in part, with coronal holes,and interplanetary coronal mass ejections). We use the taxonomy provided byZhao et al. (2009) to identify the three types of solar wind. We then map thein-situ observations to the 2.5 solar radii surface. With the aid of thepotential-field-source surface model (PFSS), we calculate the normal distancefrom the solar wind "foot point" to the local helisopheric current sheet onthat surface. We find that the source region of the streamer stalk wind isnarrower compared to the previous minimum. The area outside the streamer stalkis accordingly larger, but the magnetic field strength is observed to be lower,with the result that the total amount of the magnetic open flux from theoutside of streamer stalk region is conserved in the two successive solarminima. The implications of the conservation of open magnetic flux for modelsof the behavior of the solar magnetic field are discussed.

Comparison of Two Solar Minima: Narrower Streamer Stalk Region and Conserved Open Magnetic Flux in the Region Outside of Streamer Stalk