Comparison of Stream Interactions between Observation and ENLIL Model

Details Comparison of Stream Interactions between Observation and ENLIL Model Comparison of Stream Interactions between Observation and ENLIL Model

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh11a0260j&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH11A-0260

Physics

7509 Corona, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162), 7599 General Or Miscellaneous, 7959 Models

Scientific paper

When fast stream overtakes slow stream in the solar wind, a pressure ridge forms between them to accelerate the slow stream and decelerate the fast stream. The height of this pressure ridge is a measure of the strength of the interaction. We have examined the pressure ridges at 1 AU in the ecliptic plane at stream interactions over a full solar cycle. We find that the solar wind stream structure is surprisingly constant over the solar cycle with a minimum annual average pressure of about 133 pPa and a maximum of about 231 pPa. To understand the radial evolution of these structures, we compare our results with the ENLIL 3D MHD model of the heliosphere installed at the CCMC. This model solves for plasma mass, momentum, energy density, and magnetic field, using a Total-Variation-Diminishing Lax-Friedrichs (TVDLF) algorithm. We find that the current version of the model underestimates the pressure maxima observed in stream interaction ridges. However, some general trends in the parameters are reproduced, suggesting adjustments in the grid resolution or assumed solar wind parameters may improve the comparisons.

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