Radial alignment simulation of solar wind streams observed by Pioneers 10 and 11 in 1974

Details Radial alignment simulation of solar wind streams observed by Pioneers 10 and 11 in 1974 Radial alignment simulation of solar wind streams observed by Pioneers 10 and 11 in 1974

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...10012251p&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 100, no. A7, p. 12,251-12,260

Statistics

Applications

8

Alignment, Pioneer 10 Space Probe, Pioneer 11 Space Probe, Solar Wind, Streams, Magnetohydrodynamic Flow, Magnetohydrodynamics, Solar Corona, Solar Rotation, Two Dimensional Models

Scientific paper

A particularly favorable radial lineup between spacecraft in Earth orbit and Pioneers 10 and 11 (near the ecliptic plane at approximately 5.5 AU and approximately 4.5 AU, respectively) occurred in mid-1974, when the solar corona was in a stable and well-defined warped-dipole configuration. The radial alignment study reported here differs from previous applications of the technique in two respects: (1) It is the first time a two-dimensional (2-D) MHD model has been tested over such a lengthy propagation interval; the 2-D capability is crucial for treatment of the nonradial shearing motions occurring across the stream interface. (2) The three-dimensional (3-D) structure observed in the white light corona at that time is related to the systematic patterns of nonradial flow deflections appearing at the Pioneer corotating interaction region (CIR) fronts. Comparison of predicted and observed flows for pairs of streams in two successive rotations reveals that when the parent coronal hole projects far across the solar equator in a predominantly north-south orientation (i.e., nearest the 2-D idealization), the mapping is accurate down to details of the flow structures. But where the spacecraft tracks along a latitudinal boundary of a hole or the associated stream front is inclined at a shallow angle to the equator, the numerical projections deviate systematically from the observations. Among the sources of error are 3-D dynamical interactions neglected in the model, differential rotation effects, and slow temporal evolution of the coronal structures. A characteristic pattern of north-south and east-west deflections indicative of the 3-D geometry appears across the CIRs, but these patterns evidently reflect primarily the local, as opposed to global, orientation of the 3-D stream fronts. Such patterns appear common in CIRs observed by Pioneer during this period. These findings thus hold special relevance for the analysis of Ulysses observations, since the present coronal configuration is similar to that of 1974.

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