Laboratory simulation of very strong magnetosphere's compression by giant Solar flare's plasma, supplying a SEP's trapping and other world wide effects
Abstract
The problems of required conditions and possible consequences of the super - compression (up to R_m∼ 3R_E) of the Earth's magnetosphere by giant CME are investigated by the methods of laboratory and computer simulations. A useful relation between an expected magnetopause location R_m^* and the kinetic plasma energy E_0 of spherical plasma cloud (exploded at distance R_0) was obtained R_m^*/R_0≈ 0,75/ae^{1/6} and tested by MHD - model of Nikitin & Ponomarenko (1994) with the using their main energetic criterion of the problem {ae=3E_0 R_0^3/μ^2 (for magnetic moment μ of point obstacle in vacuum). This relation could describe rather well an observed compression (R_m∼ 5-6 R_E for CME with energy 10^{32} ergs and effective value E_0∼ 10^{33} ergs, into 4π) and predicts R_m^*≤ 3R_E in a probable case of Mega Flare with the total energy release ∼ 10^{34} ergs and possible E_0∼ 5\cdot 10^{34} ergs according to Kane et al. (1995) and Tsurutani et al. (2003). Some most important features of the formation such Artificial Magnetosphere (AM) structure and its possible influence onto various geospheres media (or technosphere areas) could be successfully studied in the simulative experiments at KI-1 facility of ILP with Laser Plasmas (LP) of E_0 up to kJ and dipole μ∼ 10^7 G\cdot cm^3 as was shown by Ponomarenko et al. (2001) and Zakharov (2003). But the main problem of such planned AMEX experiment (at ae∼ 50 for R_0=75 cm) is the influence of finite value of ion magnetization ɛ_m=R_L/R_m^* based on the ion Larmor radius R_L=mcV_0/ezB_d, where V_0∼ 100 km/s is the expansion velocity of LP and B_d is the initial dipole field at the point R_m^*. Of coarse, ɛ_m≪ 1 in a real space conditions (excluding cases of Mercury or asteroids, explored by Omidi et al. (2004)) while in the laboratory to fulfill both need constrains ae≫ 1 and ɛ_m≪ 1 we should use a thermonuclear plasma and devices. To overcome this problem we did a 3D/PIC - calculations by hybrid model of Kyushu University, described by Muranaka et al. (2001), to find out a critical value of ɛ_m^* (≈ 0,2-0,3), which need for MHD - like interaction of exploding plasmas with magnetic dipole.
- Publication:
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Solar Activity and its Magnetic Origin
- Pub Date:
- 2006
- DOI:
- Bibcode:
- 2006IAUS..233..389P