Like the solar photons the solar wind particles induce a drag force onto the zodiacal dust grains in the heliosphere. For the distant solar wind with high Mach numbers the drag coefficient is a constant, but close to the Sun, where Mach numbers become small, the drag coefficient is a complicated function of the ion sound speed, density and temperature. We discuss the dynamics of dust particles ...

The solar wind-magnetosphere system is nonlinear. The solar wind drivers of geosynchronous electrons with energy range of 1.8–3.5MeV are investigated using mutual information, conditional mutual information (CMI), and transfer entropy (TE). These information theoretical tools can establish linear and nonlinear relationships as well as information transfer. The information transfer from solar wi...

One possibility for propellantless propulsion in space is to use the momentum flux of the solar wind. A way to set up a solar wind sail is to have a set of thin long wires which are kept at high positive potential by an onboard electron gun so that the wires repel and deflect incident solar wind protons. The efficiency of this so-called electric sail depends on how large force a given solar win...

Distributed generation (DG) plays a vital role in electrical power networks. However, loss reduction, voltage profile improvement, friendly environment, and reliability are all benefits of DG units. In this research work, worthwhile methodology is recommended for optimal allocation traditional (gas turbine) renewable energy sources that based on distributed generators which include solar wind t...

The fraction of solar wind which interacts with the dayside ionosphere and atmosphere of Venus was calculated assuming the presence ofmagnetic field fluctuations in the, • ionosheath region and taking into consideration the interaction with the upper neutral atmosphere extending above the ionopause. The Monte Carlo calculations indicated that fluctuations with Brms/(B) of 0.3, a not unreasonabl...

We resolve the paradox that although magnetic collimation of an isotropic solar wind results in an enhancement of its proton flux along the polar directions, several observations indicate a wind proton flux peaked at the equator. To that goal, we solve the full set of the timedependent MHD equations describing the axisymmetric outflow of plasma from the magnetized and rotating Sun, either in it...

The effect of solar rotation on the proton-alpha differential flow speed, vαp, and consequently on the angular momentum transport in the solar wind, is explored. Using a 3-fluid model, it is found that the radial component of the momentum equation for ions is modified by the force introduced by the azimuthal components. This force plays an important role in the force balance in interplanetary s...

This paper describes the principal features of 24 hr averages of the magnetic field strength variations B(t) and their relationships to the plasma and energetic particles observed prior to and after the crossing of the termination shock (TS) by Voyager 2 (V2). The solar wind (pre-TS crossing) and heliosheath (post-TS crossing) data extend from day of year (DOY) 1 through 241, 2007 and from 2007...

[1] On April 13 (day 103), 2001, 0700–1400 UT, the Polar satellite experienced different plasma regimes (i.e., magnetosphere, magnetosheath, and solar wind) because of the solar wind dynamic pressure variations and its high orbital inclination near the subsolar magnetopause meridian. When Polar was in the magnetosheath, quasiperiodic spacecraft potential (SP) variations, corresponding to densit...

We study the formation and evolution of a turbulent spectrum of Alfvén waves driven by reflection off the solar wind density gradients, starting from the coronal base up to 17 solar radii, well beyond the Alfvénic critical point. The background solar wind is assigned and 2D shell models are used to describe nonlinear interactions. We find that the turbulent spectra are influenced by the nature ...