LFM-helio MHD model and comparisons with Ulysses Fast Latitude Scan data

Details LFM-helio MHD model and comparisons with Ulysses Fast Latitude Scan data LFM-helio MHD model and comparisons with Ulysses Fast Latitude Scan data

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh13b1532p&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH13B-1532

Physics

[2100] Interplanetary Physics, [2102] Interplanetary Physics / Corotating Streams, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

We present results from a newly developed heliospheric magnetohydrodynamic (MHD) model. We have adapted the Lyon-Fedder-Mobarry (LFM) magnetospheric MHD code to the heliospheric plasma and fields to create the LFM-helio model. The results of the simulations illustrate the quality of MHD solutions obtained by this model. We have simulated a steady state inner heliosphere for Carrington rotations (CR) 1891 through 1895. These CRs constitute a segment of the declining phase of solar cycle 22 and correspond to the fast latitude scan performed by Ulysses in 1995 . The inner boundary condition, at 0.1 AU, is obtained using the Wang-Sheeley-Arge (WSA) model. For these runs, the LFM-helio solution domain is a sphere out to 2 AU, excluding 10° cones centered on the poles, in 2°x2°x2 Rsolar resolution, which encompasses the pertinent segment of the Ulysses orbit. We have also made some higher resolution runs. We explore spatial structures in the solar wind velocity field for these and a few other CRs during the solar cycle and investigate sector structure, shocks, and corotating interaction regions (CIRs) using the fine scale features captured by LFM-helio. We compare the simulation results for magnetic field, plasma number density and temperature to concurrent Ulysses in situ data as well as to results from previous models, such as the one described in Riley et al. (JGR 2001).

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