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Solar Wind Heating and Turbulence

Objective

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.

Coordinator

ECOLE POLYTECHNIQUE
Net EU contribution
€ 264 668,40
Address
Route De Saclay
91128 Palaiseau Cedex
France

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Region
Ile-de-France Ile-de-France Essonne
Activity type
Higher or Secondary Education Establishments
Non-EU contribution
€ 0,00

Partners (1)

Partner

Partner organisations contribute to the implementation of the action, but do not sign the Grant Agreement.

THE REGENTS OF THE UNIVERSITY OF CALIFORNIA
United States
Net EU contribution
€ 0,00
Address
Franklin Street 1111 12 Floor
94607 Oakland Ca

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Activity type
Higher or Secondary Education Establishments
Non-EU contribution
€ 172 130,40