Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh41b..07p&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH41B-07
Astronomy and Astrophysics
Astrophysics
[7500] Solar Physics, Astrophysics, And Astronomy, [7959] Space Weather / Models
Scientific paper
We have used the Lyon-Fedder-Mobarry (LFM) heliospheric magnetohydrodynamic (MHD) model, the LFM-helio, to examine the radial evolution of stream interactions during Carrington rotations (CRs) 2060 and 2068. The LFM-helio is an adaptation of the magnetospheric LFM MHD code to heliospheric plasmas and fields. For the simulations considered, the solution domain extends from 0.1 AU to 2.0 AU. The equations are solved on a uniform spherical grid, excluding 10 degree cones centered at the poles. The inner boundary conditions are obtained using the Wang-Sheeley-Arge (WSA) coronal model, which provides the velocity and magnetic field based on Global Oscillation Network Group (GONG) observations of photospheric fields. During these intervals, observations at L1 show fast and slow streams of solar wind, regions of compressed plasma and magnetic field, as well as non-radial plasma flows. Concurrently, the MErcury Surface, Space ENvironment, Geochemistry and Ranging (MESSENGER) spacecraft was orbiting the Sun at approximately ~0.40 AU and ~0.66 AU for CRs 2060 and 2068, respectively. Cruise phase magnetic field data is available. The LFM-helio model results are compared to in situ observations of magnetic field, solar wind speed and plasma density from ACE and magnetic field measurements from MESSENGER. The comparisons allow us to assess the quality of the model solution at different distances from the Sun, as well as the radial evolution of the stream interaction regions. The global nature of the LFM-helio solution facilitates the study of the steepening of the stream interaction regions and also aids in putting the in situ data into context.
Hughes W. W.
McGregor Sarah L.
Merkin V. G.
Pahud D. M.
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