Magnetopause shape as a bivariate function of interplanetary magnetic field Bz and solar wind dynamic pressure

Details Magnetopause shape as a bivariate function of interplanetary magnetic field Bz and solar wind dynamic pressure Magnetopause shape as a bivariate function of interplanetary magnetic field Bz and solar wind dynamic pressure

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9821421r&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A12, p. 21,421-21,450

Physics

178

Bivariate Analysis, Dynamic Pressure, Interplanetary Magnetic Fields, Magnetopause, Plasma Dynamics, Plasma Pressure, Solar Wind, Mathematical Models, Pressure Effects

Scientific paper

We present a new method for determining the shape of the magnetopause as a bivariate function of the hourly averaged solar wind dynamic pressure (p) and the north-south component of the interplanetary magnetic field (IMF) Bz. We represent the magnetopause (for XGSE greater than -40 RE) as an ellipsoid of revolution in solar-wind-aberrated coordinates and express the (p, Bz) dependence of each of the three ellipsoid parameters as a second-order (6-term) bivariate expansion in Inp and Bz. We define 12 overlapping bins in a normalized dimensionless (p, Bz) `control space' and fit an ellipsoid to those magnetopause crossings having (p, Bz) values within each bin. We also calculate the bivariate (Inp, Bz) moments to second order over each bin in control space. We can then calculate the six control-space expansion coefficients for each of the three ellipsoid parameters in configuration space. From these coefficients we can derive useful diagnosis of the magnetopause shape as joint functions of p and Bz: the aspect ratio of the ellipsoid's minor-to-major axes; the flank distance, radius of curvature, and flaring angle (at XGSE = 0); and the subsolar distance and radius of curvature. We confirm and quantify previous results that during periods of southward Bz the subsolar magnetopause moves inward, while at XGSE = 0 the flank magnetopause moves outward and the flaring angle increases.

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