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3 the Magnetosphere 3-1 Formation of the Magnetosphere and Magnetospheric Plasma Regime

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3 the Magnetosphere 3-1 Formation of the Magnetosphere and Magnetospheric Plasma Regime 3 The Magnetosphere 3-1 Formation of the Magnetosphere and Magnetospheric Plasma Regime OBARA Takahiro The Earth's magnetosphere is formed by the plasma flow from the Sun; i.e. solar wind. This solar wind particle can enter the magnetosphere through non-MHD processes and pro- duces specific regions of plasma. This is due to the convection motion seen in the magne- tosphere. An enhancement of the magnetospheric convection causes storms and sub- storms in the magnetosphere. Highly energetic particles can be produced through very effi- cient acceleration processes during the storms. In this paper we describe the fundamental physics of the magnetosphere, aiming a transition of researches to the Space Weather fore- cast. Keywords Magnetosphere, Plasma, Magnetospheric convection, Storms and substorms, Ener- getic particles 1 Outline of the Formation of the in the southern hemisphere. Magnetosphere and the Mag- There is an influx of solar wind plasma netospheric Plasma Structure particles in the lobe region. The area of the lobe near the magnetopause is referred to as The magnetosphere is a distinct region in the mantle. The magnetic field intensity is space surrounding the Earth, and its structure low near the equatorial plane, where the north- has been the subject of numerous detailed ern and southern lobes meet. Hot plasma satellite observations. Fig.1 shows a represen- accumulates in this region, referred to as the tation of this structure, with the upper front plasma sheet. Characteristic plasma regimes quarter removed to show the interior. The are present near the Earth, with plasma with Earth is at the center, and the solar wind flows higher energies relative to the plasma sheet. from left to right. The front (dayside) of the These regimes surrounding the Earth form the magnetosphere is compressed, while the ring current that causes magnetic storms; these nightside is stretched, forming the tail of the regimes also form the Van Allen radiation magnetosphere (magnetotail). First let us belts. Near the Earth, upward diffused ionos- define the names of the magnetospheric com- pheric plasma forms the plasmasphere. The ponents. The magnetosphere is the region plasmasphere has a clear external boundary inside the magnetopause. The wide structure referred to as the plasmapause. on the north and south sides of the equatorial The plasma regimes studied in this paper plane is referred to as the lobe. Here, the consist of: (1) the boundary layer, featuring magnetic field lines extending from the polar particles resembling those in the solar wind; regions of the Earth are stretched toward the (2) the plasma sheet, consisting of medium- nightside. The magnetic field lines are earth- energy particles (several keV); (3) the inner ward in the northern hemisphere and tailward magnetosphere, consisting of high-energy par- OBARA Takahiro 61 ticles (> 10 keV); and (4) the plasmasphere, regions of the solar wind, and thus, a shock consisting of cold plasma. When grouped structure is formed. Such shocks, on the exte- according to plasma origin, (1), (2), and (3) rior of magnetopause, have been confirmed are plasmas originating in the solar wind, and through satellite observations. These shocks generally, particles nearer the Earth have high- are referred to as the bow shock, due to the er energies. In contrast, (4) is plasma originat- overall structure's similarity to waves created ing from the Earth. These regimes are not by the bows of ships. completely isolated from each other; they The magnetosheath is the region between coexist and interact. the bow shock and the magnetopause. The The followings are the terms used in this plasma in this region has properties similar to paper in the explanation of magnetospheric those of the solar wind plasma, but in this physics. As seen from the Earth, the magne- region the plasma is heated upon crossing the tosphere on the sunward side is referred to as bow shock. The plasma flow inside the mag- the dayside magnetosphere, and the opposite netosheath is slightly slower than the solar side is referred to as the nightside magneto- wind velocity, and on the whole, this flow is sphere. Similarly, we will use the terms deflected along the magnetopause surface. "dawn" and "dusk" sectors. Fig.1 shows the Simulations have been conducted on the direc- magnetosphere as seen from the dusk sector. tion of the solar wind magnetic field in the The characteristic feature of the nightside magnetosheath based on gas-dynamic theory magnetosphere is the tail, which is elongated and on MHD (magnetohydrodynamics), and over a great distance; this structure is referred the models have been found to be consistent to as the magnetotail. with observations. 2.2 Magnetopause Region When the supersonic plasma flow from the sun (solar wind) collides with the geomagnetic Bow Plasma Shock Interplanetary Lobe Mantle field, its front (dayside) region is compressed, Magnetic Field (IMF) and a clear boundary is formed. The solar Plasma Sheet wind dynamic pressure and the magnetospher- Plasmasphere Ring Current ic magnetic pressure are balanced at this Solar plane, which is referred to as the magne- Wind Magnetopause topause. The distance from the center of the Magnetosheath Earth to the magnetopause is approximately Fig.1 Structure of the Earth's magneto- 11 Re (Radius of Earth). When the solar wind sphere dynamic pressure increases, the magnetopause comes closer to the Earth. To conduct a 3-D simulation of the magne- 2 Influx of Solar Wind Particles topause, it is necessary to estimate the precise and External Plasma Regimes pressure distribution in the solar wind. The solar wind essentially circumvents the Earth. 2.1 Magnetosheath Particles Detailed estimations were made of the stress The solar wind is a supersonic flow. The perpendicular and parallel to the magne- Earth moves through the solar wind plasma at topause surface, and the results of these esti- supersonic speeds, in a system moving within mations are shown in Fig.2. Two interesting the solar wind. The effects of deceleration structures can be observed to the north and and compression of the solar wind as it col- south. All magnetic field lines converge at a lides with the magnetosphere cannot be trans- single point, where the magnetic field intensi- mitted at sonic velocities to the upstream ty is zero. This neutral point is referred to as 62 Journal of the Communications Research Laboratory Vol.49 No.3 2002 the cusp. The cusp is important in driving the solar wind particles. In this manner, large magnetospheric convection, as will be dis- amounts of both momentum and magnetic cussed in detail in a later section. field flux accumulate in the nightside magne- tosphere. How do the reconnections of the magnetic field lines occur? Fig.4 shows a pair of mag- netic field lines in the reverse directions posi- tioned above and below a plane perpendicular to the page (a magnetic neutral plane). When they are pushed closer to each other, a current is generated at the boundary, in accordance with Ampere's law. This current is referred to as a neutral sheet current. If conductivity is assumed to be infinite, then a barrier of stronger current is created as the magnetic Fig.2 The 3-D structure of the magne- topause. Solid and dashed lines repre- field lines approach each other, and the field sent magnetic field lines and magne- lines remain isolated. However, if resistance topause currents, respectively. (Midgely, 1963) is created somewhere on the neutral plane, then the energy of the magnetic field is con- The magnetosphere is a region usually sumed at that point. Magnetic field lines near shielded from solar wind particles. Most of the point migrate toward this point to compen- the solar wind particles are deflected away sate for the energy loss. In Fig.4(c), X repre- from the Earth, but during a southward solar wind magnetic field, there is a large injection of energy into the magnetosphere. This theory Magnetic met with wide attention when it was first pro- Field Lines Neutral Sheet Current posed by Dungy (1963). As shown in Fig.3, Neutral Sheet when the solar wind magnetic field is oriented southward, reconnection of the magnetic field lines occurs in the dayside magnetopause. A terrestrial magnetic field line that has been connected to a solar wind magnetic field line becomes open and migrates downstream (to the nightside). The momentum of the solar wind enters the magnetosphere along with Point Point Fig.3 In the dayside magnetopause, the magnetic field lines are reconnected to interplanetary magnetic field (IMF) Fig.4 Schematic diagram of reconnection lines. Magnetic field lines migrate of magnetic field lines along the lines numbered 1－8 OBARA Takahiro 63 sents the point at which magnetic field lines has revealed that the region of electron injec- converge and are reconnected. Fig.4(d) shows tion is located near the equatorial region the new pair of magnetic field lines resulting (reconnection region of magnetic field lines) from the reconnection. in the dayside magnetosphere. Satellites crossing the cusp in the south- 2.3 Cusp Particles north direction have observed ions drifting The high-latitude region of the dayside toward high-latitude regions as they precipi- magnetosphere features a characteristic mag- tate. This phenomenon, where ions with netic field configuration. This structure, lower precipitation energies drift to higher lat- called the cusp, is located at the boundary itudes, can be explained by the presence of between the closed magnetic field lines on the tailward convection in the polar cap (region dayside and the magnetic field lines that surrounded by auroras). reconnect with the solar wind magnetic field and stream toward the tail. There is direct 2.4 Mantle Particles downward injection of solar wind plasma As shown in Fig.5, the magnetosheath toward the Earth at the cusp region (solid plasma penetrates into the lobes and creates a black region in Fig.5(a)).
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