Tail Lobe Revisited: Magnetic Field Modeling Based on Plasma Data

Details Tail Lobe Revisited: Magnetic Field Modeling Based on Plasma Data Tail Lobe Revisited: Magnetic Field Modeling Based on Plasma Data

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999stin...0273458k&link_type=abstract

Technical Report, PB2002-105057; IRF-SR-260

Physics

Dynamic Pressure, International Sun Earth Explorer 1, Interplanetary Magnetic Fields, Magnetic Effects, Wind Pressure, Magnetosheath, Magnetometers, Solar Wind, Boundary Layers, Plasmas (Physics)

Scientific paper

Plasma data from the ISEE-1 and -2 spacecraft during 1977-1980 have been used to determine the distribution of data points in the magnetotail in the range of distances -20 < XGSM < --15, i.e. which of the records that were located in the current sheet, in the tail lobe, in the magnetosheath and in the boundary layers respectively. The ISEE-1 and -2 magnetic field data for the records in the tail lobe were then used to model the tail lobe magnetic field dependence on the solar wind dynamic pressure, on the Interplanetary Magnetic Field (IMF) and on the Dst index. The tail lobe magnetic field was assumed to be dependent on the square root of the dynamic pressure based on the balance between the total magnetic pressure in the tail lobes and the dynamic pressure of the solar wind. The IMF dependent terms, added to the pressure term, were sought in many different forms while the Dst dependence of the tail lobe magnetic field was assumed to be linear. The field shows a strong dependence on the square root of the dynamic pressure and the different IMF dependent terms all constitute a significant contribution to the total field. However, the dependence on the Dst index turned out to be very weak at those down-tail distances. The results of this study are intended to be used for parameterizing future versions of the data-based models of the global magnetospheric magnetic field.

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