Computer Science – Numerical Analysis
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....9914747l&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. A8, p. 14,747-14,760
Computer Science
Numerical Analysis
16
Curves (Geometry), Heliosphere, Magnetic Fields, Magnetohydrodynamic Waves, Mathematical Models, Perturbation, Solar Wind, Differential Equations, Flow Stability, Flux Density, Numerical Analysis, Solar Rotation, Space-Time Functions, Wave Propagation
Scientific paper
We study a two-dimensional propagation of Alfvenic perturbations within the solar equatorial plane (SEP) in the solar wind with a spiral magnetic field. Analytical solutions within the entire frequency range are derived at large radial distance r. Numerical solutions which smoothly pass through the Alfven critical point rA are also obtained. Since the spiral magnetic field caused by the solar rotation scales as approximately 1/r at large r, the velocity and magnetic field perturbations, which are perpendicular to the SEP, remain small relative to the wind parameters in the entire radial range. The frequency criterion for the non-Wentzel-Kramers-Brillouin (WKB) radial scalings of the perturbation variables to appear is (f + mfdot in circle) squared is less than f2c, where f is the perturbation frequency, fdot in circle is the solar rotation frequency, m is the azimuthal wavenumber, and fc is the well-known characteristic frequency determined by the wind parameters. We demonstrate that the process of continuous reflection in a spiral magnetic field and the effect of superposing Alfvenic perturbations with various f and m can lead to variations of the relative magnetic field fluctuation, the normalized cross helicity sigmac, the Alfven ratio ra, the magnetic perturbation energy density Eb, and the kinetic perturbation energy density Enu, which differ from the predictions of the conventional WKB theory. In particular, the non-WKB radial scalings of the perturbation variables can appear at any timescales with appropriate values of m. The relevance of these results to data analyses on interplanetary fluctuations is discussed, and we emphasize the importance of obtaining fluctuation spectrum with respect to both f and m in the outer heliosphere.
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