Magnetotail plasma parameters pdf

The above results can provide useful information for the design and protection of lunar-orbiting spacecraft and can be used as the background magnetic field and plasma parameters in the numerical simulation of mid-magnetotail reconnection. moid in three typical plasma parameters listed in Table 1. RUN 1 is the uniform density case, RUN 2 corresponds to the near-Earth magnetotail case where the lobe plasma den-sity is very low, and RUN 3 may be one case for the distant magnetotail with the high-density mantle plasma. 3. Plasmoid Formation: Region Identi?cation The plasma environment for the NGST spacecraft will depend on its position relative to the magnetotail region of the earth's magnetosphere.* The data given here from the GEOTAIL and SOHO spacecraft give a sampling of the expected range of the solar wind parameters inside and outside of the magnetotail. The (Section 2) and Earth's magnetotail (Section 3), we may be able to ?nd similarities and differences of electron acceleration mechanisms, although both the measurement techniques and the plasma parameters are very different in each environment (Section 1.2, Appendix A). the detection of low-density and faster-than-sheath magnetospheric plasma can be taken as a marker of rolled-up vortices. This typical feature, together with quasi-periodic ?uctuations (periods of 1-5 min) in the plasma parameters and magnetic ?elds under northward IMF, can be used as criteria to identify Magnetic field and plasma observations from magnetotail passes of the AMPTE/IRM satellite are used to study the low-frequency magnetic fluctuation energy density as a function of several local plasma parameters. The plasma characteristics in the near-midnight region are described and indicate a transition between the region of the magnetosphere containing plasma on closed drift paths and that containing ?ux tubes which may not complete a full rotation around the planet. Data from the electron spectrometer reveal two plasma states of high and low density. the estimated solar wind plasma parameters upstream of Mercury [2]. We also use our model to determine the location of the magnetospheric boundaries, i.e. bow shock, magnetopause, and magnetotail, and their correlations and variations with the solar wind plasma and compare them with those previously estimated from observations [2]. As of 2014 the magnetosphere of Saturn has been directly explored by four spacecraft. The first mission to study the magnetosphere was Pioneer 11 in September 1979. Pioneer 11 discovered the magnetic field and made some measurements of the plasma parameters. parameter for the applicability of this method. The E B =0 approximation is rather good for those whistler mode waves crossed the magnetotail at about 17R E inside the plasma sheet, near the magnetic equator, during a substorm event. The most probable main periods of the magnetic ?eld and plasma parameters are between 143 s and 160 s, which are located in the frequency band of Pi2 and Pi3 pulsations. The second and third period ranges from 63 s to 70 s and from 34 s to 37 s, respectively. Main periods of these parameters change little with the radial distance. pdf. Oscillatory flow braking in the magnetotail: THEMIS statistics the normal component of the magnetic ?eld BZ Major plasma parameter changes occurred during the ?rst (note that the difference between BZ at P4 and the one several periods of oscillating ?ow (between about 9:18 and pdf.