MHD Modeling of supersonic, super-alfvenic distrubances propagating in the interplanetary plasma and their relationship to the geospace environment

Wavelet Analysis of Big Data in the Global Investigation of Magnetic Field Variations in Solar-Terrestrial Physics

“…The precise understanding of these phenomena requires the joint efforts of astronomers and geophysicists. All this indicates that knowing and predicting geomagnetic storms depends on knowing the propagation of interplanetary disturbances as a hydrodynamic process in three dimensions, [32]. For example, it has been found that the direction of the interplanetary magnetic field (IMF) vector B is essential to unlock the geomagnetic storm mechanism.…”

“…It would be interesting for the unexperienced reader to hear about the parameters of a simulated Coronal Mass Ejection (CME), see details in [32], where a magnetohydrodynamic model is numerically implemented: the release energy is E, = 6.0 × 10 22 J; the release mass is M, = 2.5 × 10 10 kg; the initial velocities of the ejected flow are: the radial u d = 1500 km / sec. and the tangential is v d = 0; the duration of CME is 180 seconds; the angle of the small conic area associated with the CME is 27 0 , see a model with these realistic parameters simulated in [32]. To understand how the southern direction of the interplanetary magnetic field is formed, we will look at the results of Figure 3: ... the computer modeling of the disturbance propagation in the interplanetary environment caused by the CME.…”

“…To understand how the southern direction of the interplanetary magnetic field is formed, we will look at the results of Figure 3: ... the computer modeling of the disturbance propagation in the interplanetary environment caused by the CME. As more details are provided in [32], let us shortly describe the dynamics of the simulated disturbance propagation in the interplanetary medium: After the CME happens at t = 0 and has duration 3 min., about 40 hours later the disturbance reaches Earth's orbit and (see Figures 3, 4 below and the Figures in [32]).…”

“…On Figure 9 we provide the tangential velocity V of the disturbed solar wind at 40 hours after the CME; the values of V are dimensionless: What concerns the magnetic field, we refer to the paper [32], where a detailed figures of the disturbed tangential IMF B z are provided. In [32] it is seen that the tangential component of the magnetic field vector B t (which in fact coincides with the B z component in the geocentric Cartesian coordinate system) also has positive and negative values. Thus a structure is formed in which the direction of the disturbed magnetic field vector is changing to the north or to the south (in the same coordinate system mentioned above).…”