Turbulence vs kinetic instabilities

Two dimensional expanding box hybrid simulations clearly demonstrate
that kinetic instabilities may coexist with strong plasma turbulence and bound the plasma parameter space. Read more

Estimating proton heating related with turbulence in the solar wind by means of high-resolution hybrid simulations

A very high accuracy - i.e., a very high spatial resolution, a large number of particles and a fine-tuned choice of the main numerical parameters - is mandatory when trying to obtain a quantitative estimate for the perpendicular proton temperature by means of hybrid simulations, and to draw any firm conclusion about the development of a preferential proton heating.  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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Sodium gyro-resonance with Kelvin-Helmholtz waves at Mercury.

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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

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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Quasi-Trapped Particles in the Hermean Magnetosphere

Mercury has its own magnetic field as has been revealed by Mariner 10 in 1970's and confirmed by NASA's MESSENGER mission recently. Even if the planetary magnetic dipole strength is about 2500 times smaller, it is sufficient to form magnetosphere structure similar to the Earth's magnetosphere. Due to the minimum data from in-situ measurements, there are lot of open questions on the magnetospheric properties and processes. Global numerical simulations helps to address and answer some of them. Simulations proved useful for predictions of features to be investigated using real data and they give global context to local measurements. Read more