Electron energetics in the expanding solar wind

Detailed statistical analysis of electron energetic properties as measured by HELIOS 1&2 spacecraft indicates that for the non-adiabatic cooling of electrons in the expanding solar wind no significant external heating mechanisms are required. Read more

Recovering features of the observed solar wind spectra by means of high-resolution hybrid simulations

High-resolution two-dimensional hybrid simulations of turbulence with an out-of-plane ambient magnetic field are able to simultaneously reproduce several aspects of observed solar wind spectra over a large range of scales, from the MHD to the sub-ion kinetic range.
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The imprints of expansion on solar wind turbulence

Numerical simulations show that solar wind expansion affects the evolution of turbulence in the heliosphere, causing the emergence of strong transverse magnetic fields and of radial velocity jets. Read more

Electron heat flux in the solar wind: Data vs. Simulations

Numerical simulations, which include the effects of binary collisions, are able to reproduce qualitatively and quantitatively the electron heat flux in the solar wind observed at 1 AU. Read more

Proton and alpha particle thermal energetics in the solar wind

Numerical simulations indicate that proton and alpha particle thermal energetics in the solar wind are importantly influenced by kinetic instabilities. Read more

The role of binary collisions in the electron properties of the solar wind

Numerical simulations show that the effect of the radial expansion and the binary collisions between electrons play a significant role in shaping the observed velocity distribution function. Read more

MHD Simulations of the Hermean Magnetosphere

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Solar Wind – Time Development of Waves

The solar wind is a high flow of plasma from the Sun which fills the solar system. As the solar wind flows away from the Sun it expands, and this expansion changes the particle distribution function within the plasma. This can only happen because the plasma is very low density and very high temperature so that it is collisionless, which means that the particle distribution functions are not forced to be stable Maxwellian distributions as in a normal gas. Read more