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The impact of the solar wind onto the magnetosphere generates an electric field within the inner magnetosphere (r < 10 a; with a the Earth's radius) - the convection field-. Its general direction is from dawn to dusk. The co-rotating thermal plasma within the inner magnetosphere drifts orthogonal to that field and to the geomagnetic field Bo. The generation process is not yet completely understood.〔Pukkinen, I., et al. (eds.): "The Inner Magnetosphere: Physics and Modelling", Geophysical Monograph AGU, Washington, D.C., 2000〕 One possibility is viscous interaction between solar wind and the boundary layer of the magnetosphere (magnetopause). Another process may be magnetic reconnection. Finally, a hydromagnetic dynamo process in the polar regions of the inner magnetosphere may be possible. Direct measurements via satellites have given a fairly good picture of the structure of that field.〔Heppner, J.P., in Dyer (ed): "Critical Problems of Magnetospheric Physics", Nat.Akad. Sci., Washington, DC., 107, 1972〕〔Iijima, T. and T.A. Potemra, J. Geophys. Res.,83, 599, 1978〕 A number of models of that field exists.〔McIlwain, C.E., Adv. Space Sci., 6, 187, 1986〕〔Richmond, A.D., and Y. Kamide, J. Geophys. Res., 93,5741, 1988〕〔Weimer, D.R., Geophys. Res. Lett., 23, 2549, 1996〕〔Maynard, N.C., and A.J. Chen, J. Geophys. Res., 80, 2009, 1975〕 A widely used model is the Volland-Stern model 〔Volland, H., J. Geophy. Res. 78, 171, 1973〕〔Stern, D., J. Geophys. Res. 80, 595, 1975〕 〔Burke, W.J., ''The Physics of Space Plasmas'', Boston College, ISR, Boston, 2012〕 ==Model Description== It is based on two simplifying assumptions: first, a coaxial geomagnetic dipole field B is introduced. Its magnetic field lines can be represented by the shell parameter with r the distance from the Earth, a the Earth's radius, and θ the co-latitude. For r = a, θ is the co-latitude of the foot point of the line on the ground. L = const is the equation of a magnetic field line, and r = a L is the radial distance of the line at the geomagnetic equator (θ = 90°). Second, it is assumed that the electric field can be derived from an electrostatic potential Φc. Since in a highly conducting electric plasma like the magnetosphere, the electric fields must be orthogonal to the magnetic fields, the electric potential shell is parallel to the magnetic shell. The relation \left(\frac\right)^q\sin(\tau-\tau_\mathrm)|}} fulfills that condition. Here is the separatrix〔Vasyliunas, V. M., in B. M. McCormac(ed.), "Particles and fields in the magnetosphere", D. Reidel, Dordrecht, 1970〕 separating the low latitude magnetosphere with closed geomagnetic field lines at θ ≥ θm from the polar magnetosphere with open magnetic fieldlines (having only one footpoint on Earth), and τ the local time. θm ~ 20° is the polar border of the auroral zone. q, Φco, and τco are empirical parameters, to be determined from the observations. Eq.() yields for a coordinate system co-rotating with the Earth, its geomagnetic equator being identical with the geographic equator. Since the electric potential is symmetric with respect to the equator, only the northern hemisphere needs to be considered. The general direction of the potential is from dawn to dusk, and Φco is the total potential difference. For a transformation from a rotating magnetospheric coordinate system into a non-rotating system, τ must be replaced by the longitude -λ. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Magnetospheric electric convection field」の詳細全文を読む スポンサード リンク
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