Topology of Magnetic Ejecta at 1 AU

Details Topology of Magnetic Ejecta at 1 AU Topology of Magnetic Ejecta at 1 AU

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21a..03h&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH21A-03

Physics

3210 Modeling, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks, 2164 Solar Wind Plasma

Scientific paper

We discuss several magnetic ejecta events of possible solar origins, including magnetic clouds, driving interplanetary shocks as observed by the ACE spacecraft at 1 AU. The shock normals are analyzed using the nonlinear least squares fitting of the Rankine-Hugoniot relations, along with preaveraged coplanarity methods. The axis (z) of a magnetic cloud, modeled as a cylindrical magnetohydrostatic structure, is determined from the single-spacecraft data along its trajectory across the structure. Namely, from the definition of a magnetic potential vector A=A {\hat z}, the transverse magnetic fields are governed by the Grad-Shafranov (GS) equation, ∇ t2 A=-μ 0 dPt/dA, where Pt(A)=p(A)+B_z2(A)/2μ0_. The optimal z axis is found by minimizing the fitting residue of function Pt(A). Such axes are then compared with the associated shock normals, and their relative orientation in space is discussed. Furthermore, the cross-section of a magnetic cloud can be obtained by solving the GS equation, showing non-axisymmetric and helical field structure characteristic of a magnetic flux rope that might be related to shock properties. Magnetic topology of complex ejecta (Burlaga et al., 2001) lacking the features of magnetic clouds is also recovered approximately by the GS reconstruction technique. The results show highly irregular configurations with possible implications of interaction and distortion. Finally, an event study from two-spacecraft measurements is presented to illustrate the validity of the technique. (The research is supported by NASA grant NAG5-6912.)

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