The Effects of Streams and Microstreams on the Large- and Small-Scale Heliospheric Magnetic Field

Even in nominally uniform solar wind flows, such as over the poles at solar minimum, there are substantial variations in the wind speed. We have shown previously that these are important in shearing the fluctuations in magnetic and other quantities, producing transverse wave vector variations even if the Sun produced purely radially aligned plane waves. Here we extend our previous 2-D MHD simulation studies to 3-D, and report on efforts to determine the origin of phenomena such as the ``two-component" nature of the correlation function for fluctuations. We will also extend our study of field lines in the expanding heliosphere to take into account microstreams and their effects on the heliospheric current sheet, flux tubes, and quasi-2-D fluctuations. The code uses a Flux-Corrected Transport algorithm in spherical coordinates.