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Introduction The Cluster mission
Abstract. The Cluster mission, ESA’s first cornerstone project, together with the SOHO mission, dating back to the first proposals in 1982, was finally launched in the summer of 2000. On 16 July and
Measurement of the rugged invariants of magnetohydrodynamic turbulence in the solar wind
Measurements of the total energy, cross helicity, and magnetic helicity of the solar wind at 1, 2.8, and 5 AU are presented. These quantities are the three rugged invariants of three-dimensional
CLUSTER – SCIENCE AND MISSION OVERVIEW
The European Space Agency's Cluster programme is designed to study the small-scale spatial and temporal characteristics of the magnetospheric and near-Earth solar wind plasma. The programme is
The Cluster mission
The Cluster mission, ESA's first cornerstone project, together with the SOHO mission, dating back to the first proposals in 1982, was finally launched in the summer of 2000. On 16 July and 9 August,
Origin and evolution of fluctuations in the solar wind: Helios observations and Helios-Voyager comparisons
Using hour-averaged data from the Helios and Voyager spacecraft, we have investigated the origin and evolution of low-frequency interplanetary fluctuations from 0.3 to 20 AU. Alfvenic fluctuations in
Scaling of the Electron Dissipation Range of Solar Wind Turbulence
Electron scale solar wind (SW) turbulence has attracted great interest in recent years. Considerable evidence exists that the turbulence is not fully dissipated near the proton scale, but continues
An instability of finite amplitude circularly polarized Alfven waves. [in solar wind and corona
A demonstration is presented that a finite-amplitude circularly-polarized Alfven wave is generally unstable in a MHD fluid. The wave decays by a four-wave coupling process in which the daughter waves
The FIELDS Instrument Suite for Solar Probe Plus
TLDR
The scientific objectives targeted by the SPP/FIELDS instrument, the instrument design itself, and the instrument concept of operations and planned data products are described.
Magnetohydrodynamic turbulence in the solar wind
Recent work in describing the solar wind as an MHD turbulent fluid has shown that the magnetic fluctuations are adequately described as time stationary and to some extent as spatially homogeneous.
Evidence for the presence of quasi‐two‐dimensional nearly incompressible fluctuations in the solar wind
Solar wind fluctuations are commonly regarded as a superposition of MHD waves primarily in the Alven mode. These MHD fluctuations are frequently assumed to possess slab or isotropic symmetry,
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