Computer Science
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..104m&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 104
Computer Science
11
Particle Emission, Solar Wind, Electric And Magnetic Fields, Solar Magnetism, Magnetohydrodynamics And Plasmas
Scientific paper
The helmet streamers that are observed to dominate the structure of the inner corona are formed by the interaction of the solar wind with coronal magnetic fields. We have simulated this interaction in three dimensions using the magnetohydrodynamic (MHD) equations. In order to create a realistic model, we use the magnetic field that is observed at the Sun's surface (deduced from daily Wilcox Solar Observatory magnetic field synoptic maps) as input, in combination with specified density and temperature profiles at the surface. A self-consistent 3D solar-wind solution is developed by integrating the MHD equations in time to steady state. Such solutions can reproduce the observed structures that are seen in coronagraph images and eclipse photographs of the corona. We compare the results obtained from our model with with an eclipse photograph of the corona on November 3, 1994. We also compare the position of the heliospheric current sheet with Ulysses observations during the period May-June 1993.
Linker Jon A.
Mikic Zoran
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