A Reassessment of the Waves + Q2D Model of Solar Wind Fluctuations Based on Simulations with a Turning Magnetic Field

Details A Reassessment of the Waves + Q2D Model of Solar Wind Fluctuations Based on Simulations with a Turning Magnetic Field A Reassessment of the Waves + Q2D Model of Solar Wind Fluctuations Based on Simulations with a Turning Magnetic Field

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh42a..04g&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH42A-04

Physics

2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma

Scientific paper

We examine a popular "two-component" model of the solar wind in light of the necessity for the assumed alignment of the components to turn along with the Parker spiral. In particular, we use a 3-D MHD spectral code to show that neither Q2D nor slab-wave components will turn their wavevectors in a turning Parker-like field. This is consistent with the need for transverse inhomogeneities in the background to create the required changes in the radial field. Combining the two components does result in a turning, but it is only through a nonlinear interaction between the components that no longer allows a clear identification of either component. Thus, we argue that while a "slab + Q2D" model may be a useful approximation for some purposes, it does not represent the underlying nature of the fluctuations and their anisotropy. Results to date are based on a static "mis-aligned" mean field, but we believe the results will hold for the turning case that we plan to implement soon.

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