Computer Science
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.278...63s&link_type=abstract
In ESA, Proceedings of the International Symposium on the Diversity and Similarity of Comets p 63-67(SEE N88-21884 14-91)
Computer Science
Cometary Atmospheres, Halley'S Comet, Interplanetary Magnetic Fields, Plasma Diagnostics, Vega Project, Computerized Simulation, Discontinuity, Magnetic Field Configurations, Solar Wind
Scientific paper
The differences of the VEGA-1 and VEGA-2 magnetic field investigations near Comet Halley are discussed. The different draping structures of the magnetic field observed by VEGA-1 and VEGA-2 are caused by variations of the solar wind parameters and of the cometary activity during this period. The magnetic field reversal region observed only during the closest approach of VEGA-1 is correlated with high energetic particle streams and ground-based observations of a disconnection event. A broad minimum of the wave activity during the inbound phase of both encounters occurs in the same region where a substantial change of the slope of the total magnetic field and of the plasma velocity takes place and where the observed neutral gas density has a discontinuity. The VEGA-1 and -2 magnetic field observations are compared with the results of 3-D MHD computer simulations. It is concluded that most of the measured variability is the result of IMF variations.
Fedder Joel A.
Lichtenegger Herbert I. M.
Luhmann Janet G.
Phillips John Lynch
Riedler Willi
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