The magnetospheric models used during the INTERBALL mission analysis

The Earth's magnetosphere global structure is conditioned by the interaction of the Solar wind and Earth's magnetic field.

Leaving a side the physical aspects of this interaction the main attention in this section is paid for magnetosphere topology, shape and positions of the magnetospheric structures boundaries.

Many various magnetospheric models can be available from the NSSDC.

For the INTERBALL project longterm mission analysis to provide the scienific scheduling the following magnetospheric models and the identification of the critical regions are used.

• Magnetic field with External Sources (Tsyganenko 1987,1989)
• Main magnetic field IGRF with 1975 - 1990/95 model coefficients.
• Near-Earth Bowshock (BS) (Fairfield et al., 1971);
• Magnetopause (MP) (Sibeck et al., 1991);
• Neutral sheet (NS) (Fairfield, 1980);
• Auroral oval (AOV) (Feldstein et al. 1967).
• Polar Cusp (CUSP) (K. Stasiewicz, 1991)
• Solar wind (SW) - the region outside BS;
• Magnetosheath (MS) - the region between BS and MP;
• Inner magnetosphere (IMS) - the region inside MP, for geocentric distances less then 10 RE (RE is the Earth radius equal to 6371.2 km);
• Boundary Layers including the LLBL (Low Latitude Boundary Layer) and the mantle (MBL) - the region inside MP at the distance of <= 1 RE from MP;
• Neutral sheet (NS) - region, centered by the simulative NS surface (Fairfield, 1980), with the thickness of 1 RE;
• Tail plasma sheet (PS) - the region, centered by the simulative NS surface, with the thickness of 6 RE in the central (midnight) part, 14 RE near the tail magnetopause;
• Radiation belt (RB) - the cavity between two surfaces, formed by the magnetic fileld lines, corresponding to two L walue: the L = 1.2 RE and L = 4.5 RE (L is the parameter of McIlwain, 1961);
• Auroral field lines (AUR) region - the funnel-shape cavity restricted by the geocentric distance of the order of 10 RE, between surfaces formed by magnetic field lines emerged from the polar and equatorial AOV borders;
• Polar cap (CAP) - the cavity, restricted by the geocentric distance of about 10 RE, outside of the surface formed by field lines emerged from the AOV polar boundary;

REFERENCES

• Fairfield D.H., Average and unusual location of the Earth's magnetopause and bow shock, J. Geophys. Res., 76, 6700-6716, 1971.
• Fairfield D.H., A statistical determination of the shape and position of the geomagnetic neutral sheet, J. Geophys. Res., 85, 775-780, 1980.
• Feldstein Ya.I., Starkov G.V., Dynamic of auroral belt and polar geomagnetic disturbances. Planet. Space Sci., 15, 209-229, 1967.
• McIlwain C.E., Coordinates of mapping the distribution of magnetically trapped particles. J. Geophys. Res., 66, 3681-3691, 1961.
• Sibeck D.G., Lopez R.E. and Roelof E.C., Solar wind control of the magnetopause shape, location and motion, J. Geophys. Res., 96, 5489-5495, 1991.
• Stasiewicz K. Polar Cusp Topology and Position as a Function of Interplanetary Magnetic Field and Magnetic Activity: Comparison of a Model with Viking and other Observations, J. Geophys. Res., 96, 15789-15800, September 1, 1991.
• Tsyganenko N.A., Global quantitative models of the geomagnetic field in the cislunar magnetosphere for different disturbance levels, Planet.Space Sci., 35, 1347-1358, 1987.
• Tsyganenko N.A., A magnetospheric magnetic field model with a warped tail current sheet, Planet.Space Sci., 37, 5-20, 1989.
• Tsyganenko N.A., Quantitative models of the magnetospheric magnetic field: Methods and results, Space Sci. Rev, 54, 75, 1990.