Computer Science
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010eguga..1213690a&link_type=abstract
EGU General Assembly 2010, held 2-7 May, 2010 in Vienna, Austria, p.13690
Computer Science
Scientific paper
We present results of numerical solution of Maxwell's equations for three dimensional (3-D) heliosphere with the heliolongitudinal and heliolatitudinal dependent radial solar wind speed for minimum epoch of solar activity. We show that the obtained spatial distributions of Br, Bφ and B? components of the interplanetary magnetic field (IMF) give a possibility to compose more realistic 3-D model of the Forbush effects and the 27-day variations of the galactic cosmic ray (GCR) intensity. Problem of intersections of the magnetic field lines is considered in case of interactions of the fast and slow streams of solar wind plasma. A possible creation of the heliolatitudinal component B? of the IMF near the helioequatorial region owing to existence of the heliolatitudinal component of the solar wind speed is discussed, as well.
Alania Michael
Modzelewska Renata
Wawrzynczak Anna
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