Summary
Observations of solar wind (SW) turbulence have usually emphasized magnetohydrodynamic (MHD) scales where the Kolmogorov scaling f −5/3 of the magnetic spectra is frequently observed. These spectra are
thought to result from strongly nonlinear interactions. However, the question as to how turbulence of the MHD scales terminates its cascade at smaller (kinetic) scales is still hotly debated. Answering this
question is indeed fundamental to understanding the processes of particle acceleration and plasma heating in the SW and in other astrophysical plasmas. This project aims at studying the mechanisms of energy dissipation in solar wind. We will use a innovative multiple approach that combines in-situ fields and particles data available from the multispacecraft missions, numerical simulations and theories to model the complex behavior of turbulence cascade at kinetic scales where it is dissipated.
thought to result from strongly nonlinear interactions. However, the question as to how turbulence of the MHD scales terminates its cascade at smaller (kinetic) scales is still hotly debated. Answering this
question is indeed fundamental to understanding the processes of particle acceleration and plasma heating in the SW and in other astrophysical plasmas. This project aims at studying the mechanisms of energy dissipation in solar wind. We will use a innovative multiple approach that combines in-situ fields and particles data available from the multispacecraft missions, numerical simulations and theories to model the complex behavior of turbulence cascade at kinetic scales where it is dissipated.
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| Web resources: | https://cordis.europa.eu/project/id/661472 |
| Start date: | 01-11-2015 |
| End date: | 31-10-2018 |
| Total budget - Public funding: | 264 668,40 Euro - 264 668,00 Euro |
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Original description
Observations of solar wind (SW) turbulence have usually emphasized magnetohydrodynamic (MHD) scales where the Kolmogorov scaling f −5/3 of the magnetic spectra is frequently observed. These spectra arethought to result from strongly nonlinear interactions. However, the question as to how turbulence of the MHD scales terminates its cascade at smaller (kinetic) scales is still hotly debated. Answering this
question is indeed fundamental to understanding the processes of particle acceleration and plasma heating in the SW and in other astrophysical plasmas. This project aims at studying the mechanisms of energy dissipation in solar wind. We will use a innovative multiple approach that combines in-situ fields and particles data available from the multispacecraft missions, numerical simulations and theories to model the complex behavior of turbulence cascade at kinetic scales where it is dissipated.
Status
CLOSEDCall topic
MSCA-IF-2014-GFUpdate Date
28-04-2024
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