Mathematics – Functional Analysis
Scientific paper
Apr 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...100.5877l&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 100, no. A4, p. 5877-5882
Mathematics
Functional Analysis
6
Convective Flow, Magnetohydrodynamic Waves, Plasma Turbulence, Solar Wind, Two Fluid Models, Variations, Functional Analysis, Magnetic Fields, Two Dimensional Models, Wentzel-Kramer-Brillouin Method
Scientific paper
Matthaeus et al. first suggested a two-component senario for solar wind fluctuations which contain both parallel propagating Alfven waves together with a population of quasi-two-dimensional turbulence. On the basis of these earlier ideas and further evidence, Tu and Marsch developed a two-component model, in which small-scale incompressible fluctuations are decomposed into Alfven waves and convective structures, in an attempt to account for observed radial evolutions of energy density, normalized cross helicity sigma c and Alfven ratios rA of solar wind fluctuations. According to a recent analysis on two-dimensional Alfvenic disturbances in the equatorial solar wind with aspiral magnetic field, we discuss the theoretical basis of this important two-component concept and further indicate necessary ingredients that a more self-consistent two-component turbulence model should contain. From the perspective of Alfvenic disturbances in the solar wind, the wave and convective components co exist in a naturally intermixed manner. Our analysis specifically describes behaviors of Alfvenic disturbances of all scales, including the intermediate ones. In a fully developed spiral magnetic field at large radii, the criterion for separating radially propagating Alfven waves and radially convective Alfvenic structures depends on whether absolute value of (f + mfs) is greater or less than the characteristic frequency fc identically equal to (FM U3/FB exp 2)1/2, where f is the perturbation frequency, fs is the solar rotation frequency, m is an integer for the azimuthal wavenumber, FM is the solar wind mass flux, FB is the radical magnetic flux, and U is the asymptotic wind speed. For typical solar wind parameters, the timescale corresponding to fc is approximately greater than 15 hours.
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