Interplanetary Structure Inferred from Solar Wind Phase Plane Orientation

Details Interplanetary Structure Inferred from Solar Wind Phase Plane Orientation Interplanetary Structure Inferred from Solar Wind Phase Plane Orientation

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh53a1486b&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH53A-1486

Statistics

2109 Discontinuities (7811), 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 7833 Mathematical And Numerical Techniques (0500, 3200), 7924 Forecasting (2722)

Scientific paper

All empirical investigations examining relationships between magnetospheric activity and solar wind plasma and IMF variations require the use of a solar wind propagation delay (SWPD) model to account for the time delay required for solar wind parcels to transit the distance from an upstream satellite to the bow shock of the Earth's magnetosphere. New, advanced models that account for SWPD have only recently superceded simple models such as the convection delay model, which assumes that solar wind phase planes have normals parallel to the Sun-Earth line, and the corotation delay model, which assumes that the normals to solar wind phase planes are oriented within the ecliptic plane and are perpendicular to the Parker spiral direction of the IMF. One of the new SWPD model was proposed by Weimer et al. [2002]. The model is based on the suggestion that solar wind phase plane normal directions can be found as a function of time if one forces agreement of IMF component variations as seen at a selected reference solar wind monitor (e.g. ACE) with corresponding variations measured at three other spacecraft (WIND, GEOTAIL, and IMP-8). Solar wind phase fronts are nearly planar surfaces on the scale of hundreds of Earth radii in which the interplanetary magnetic field (IMF) information content, i.e. IMF vector direction and magnitude, is highly correlated. Single spacecraft data can also be used to estimate solar wind phase plane orientation via constrained minimum variance analysis. A survey of phase plane normal orientation statistics compiled over the last eight years reveals that normals tend to cluster and are beamed in several distinct directions that change from one solar rotation to the next. The normal direction are not confined to the ecliptic plane. We present the results from a systematic search to find empirical connections between coronal magnetic field evolution and solar wind plasma and IMF variations in the near-Earth interplanetary medium.

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