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Solar Wind Heating and Turbulence

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.
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Coordinator

ECOLE POLYTECHNIQUE

Address

Route De Saclay
91128 Palaiseau Cedex

France

Activity type

Higher or Secondary Education Establishments

EU Contribution

€ 264 668,40

Partners (1)

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THE REGENTS OF THE UNIVERSITY OF CALIFORNIA

Project information

Grant agreement ID: 661472

Status

Closed project

  • Start date

    1 November 2015

  • End date

    31 October 2018

Funded under:

H2020-EU.1.3.2.

  • Overall budget:

    € 264 668,40

  • EU contribution

    € 264 668,40

Coordinated by:

ECOLE POLYTECHNIQUE

France