[1] We present a focused parameter study of solar wind–magnetosphere interaction for the young Sun and Earth, ∼3.5 Gyr ago, that relies on magnetohydrodynamic (MHD) simulations for both the solar wind and the magnetosphere. By simulating the quiescent young Sun and its wind we are able to propagate the MHD simulations up to Earth’s magnetosphere and obtain a physically realistic solar forcing o...

Hybrid power system can be used to reduce energy storage requirements. The influence of the Deficiency of Power Supply Probability (DPSP), Relative Excess Power Generated (REPG), Energy to Load Ratio (ELR), fraction of PV and wind energy, and coverage of PV and wind energy against the system size and performance were analyzed. The technical feasibility of PV-wind hybrid system in given range of...

At the Collm Observatory of the University of Leipzig LF D1 low-frequency total re ̄ection nighttime wind measurements have been carried out continuously for more than two decades. Using a multiple regression analysis to derive prevailing winds, tides and the quasi-2-day wave from the half-hourly mean values of the horizontal wind components, monthly mean values of mesopause wind parameters are ...

A kinetic model of the solar wind based on Kappa velocity distribution functions for the electrons and protons escaping out of the corona is presented. The high velocity particles forming the tail of these distribution functions have an enhanced phase space density compared to a Maxwellian. The existence of such velocity distribution functions have been introduced in the pioneering work of Scud...

While the fast solar wind is nerally thought to originate from coronal holes, the ~, Oa% source of the slow solar wind is only known to be associated with the highly structured and — highly variable streamer belt. There is growing evidence from multiple-station intensity scintillation measurements of solar wind velocity — usually referred to as IPS for interplanetary scintillation— that the slo...

The ow of solar wind from the Sun is bimodal. High speed, low density plasma comes from high magnetic latitude regions and low speed, high density ow from near the heliospheric current sheet (HCS). We investigate whether this bimodal ow combined with the HCS tilt controls the solar wind velocities in the outer heliosphere near solar minimum when the Sun's magnetic eld is roughly dipolar. We pre...

The 3-D structure of the solar wind is strongly dependent upon the Sun’s activity cycle. At low solar activity a bimodal structure is dominant, with a fast and uniform flow at the high latitudes, and slow and variable flows at low latitudes. Around solar maximum, in sharp contrast, variable flows are observed at all latitudes. This last kind of pattern, however, is a relatively short-lived feat...

[1] During the period 1999–2002 there have been three instances, in May 1999, March 2002, and May 2002, respectively, when the solar wind densities at 1 AU dropped to abnormally low values (<0.1 cm ) for extended periods of time (12–24 h). These longlasting low-density anomalies observed at 1 AU are referred to as ‘‘solar wind disappearance events’’ and in this paper, we locate the solar source...

[1] The solar wind interaction with a planetary atmosphere produces a magnetosphere-like structure near the planet whether or not the planet has an intrinsic global magnetic field. In the case of planets like Venus or Mars, which have no global intrinsic magnetic field but possess a significant atmosphere, a magnetosphere is induced in the highly conducting ionosphere by the time-varying magnet...

Incompressible magnetohydrodynamics is often assumed to describe solar wind turbulence. We use extended self-similarity to reveal scaling in the structure functions of density fluctuations in the solar wind. The obtained scaling is then compared with that found in the inertial range of quantities identified as passive scalars in other turbulent systems. We find that these are not coincident. Th...