This paper reviews the theoretical approaches and existing models of the solar wind interaction with the Local Interstellar Cloud (LIC). Models discussed take into account the multi-component nature of the solar wind and local interstellar medium. Basic results of the modeling and their possible applications to interpretation of space experiments are summarized. Open questions of global modelin...

We analyze and compare the ionic charge composition data for different types of the solar wind (slow wind from equatorial regions, fast wind from low-latitude coronal hole and fast wind from both south and north polar coronal hole) which the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses observed during the pole-to-pole pass of its primary mission. The implications on the electron t...

Although there is a lot known about the physics that dictates the movement of the planets and starts throughout the night sky, little is known about the medium which encompasses these heavenly bodies. Let us consider our own solar system as an example of this. The reason for the orbit of planets around the Sun has been well known for quite some time. In addition to this, the predictability of t...

In this paper we present the optimal year round production of synthetic methane fromwater electrolysis and CO2 comparing the use of solar PV systems and wind turbines on a monthly basis. The process starts obtaining electricity in a wind farm or a solar field, which is then used to produce oxygen and hydrogen in a system of electrolyzers. The oxygen is purified and stored, and the hydrogen, aft...

The interaction between Earth's magnetic field and the solar wind results in the formation of a collisionless bow shock 60,000-100,000 km upstream of our planet, as long as the solar wind fast magnetosonic Mach (hereafter Mach) number exceeds unity. Here, we present one of those extremely rare instances, when the solar wind Mach number reached steady values <1 for several hours on 17 January 20...

Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring....

In this paper a procedure for the probabilistic treatment of irradiance and wind meteorological data is reported in order to evaluate the energy potential of a given site as well as the generation of electricity from photovoltaic systems (PVSs) and wind systems (WECSs). In particular the aim of the proposed analysis of recorded meteorological data is twofold: first of all to check if the real p...

Aims. We present results of the analysis of cometary X-ray spectra with an extended version of our charge exchange emission model (Bodewits et al. 2006). We have applied this model to the sample of 8 comets thus far observed with the Chandra X-ray observatory and  spectrometer in the 300–1000 eV range. The surveyed comets are C/1999 S4 (), C/1999 T1 (McNaught– Hartley), C/2000 WM1 (...

[1] Geomagnetic activity has long been known to exhibit approximately 27 day periodicity, resulting from solar wind structures repeating each solar rotation. Thus a very simple near-Earth solar wind forecast is 27 day persistence, wherein the near-Earth solar wind conditions today are assumed to be identical to those 27 days previously. Effective use of such a persistence model as a forecast to...

[1] The kinetic properties of heavy ions in the solar wind reflect the plasma processes governing the solar wind in the heliosphere. We use Ulysses-SWICS data that resolve heavy ions in a wide range of mass-per-charge values, 2 m/q 9.33, to investigate the heavy ions and their dynamic evolution throughout the heliosphere. While at 1 AU the imprint of Coulomb collisions is known to be present in...