The multi-scale nature of the solar wind. (arXiv:1902.03448v1 [physics.space-ph])
<a href="http://arxiv.org/find/physics/1/au:+Verscharen_D/0/1/0/all/0/1">Daniel Verscharen</a> (UCL/MSSL, UNH), <a href="http://arxiv.org/find/physics/1/au:+Klein_K/0/1/0/all/0/1">Kristopher G. Klein</a> (UA), <a href="http://arxiv.org/find/physics/1/au:+Maruca_B/0/1/0/all/0/1">Bennett A. Maruca</a> (UD)
The solar wind is a magnetized plasma and as such exhibits collective plasma
behavior associated with its characteristic spatial and temporal scales. The
characteristic length scales include the size of the heliosphere, the
collisional mean free paths of all species, their inertial lengths, their
gyration radii, and their Debye lengths. The characteristic timescales include
the expansion time, the collision times, and the periods associated with
gyration, waves, and oscillations. We review the past and present research into
the multi-scale nature of the solar wind based on in-situ spacecraft
measurements and plasma theory. We establish the notion that couplings of
processes across scales are important for the global dynamics and
thermodynamics of the solar wind. We describe methods to measure in-situ
properties of particles and fields. We then discuss the role of expansion
effects, non-equilibrium distribution functions, collisions, waves and
turbulence, and kinetic microinstabilities for the multi-scale plasma
evolution.
The solar wind is a magnetized plasma and as such exhibits collective plasma
behavior associated with its characteristic spatial and temporal scales. The
characteristic length scales include the size of the heliosphere, the
collisional mean free paths of all species, their inertial lengths, their
gyration radii, and their Debye lengths. The characteristic timescales include
the expansion time, the collision times, and the periods associated with
gyration, waves, and oscillations. We review the past and present research into
the multi-scale nature of the solar wind based on in-situ spacecraft
measurements and plasma theory. We establish the notion that couplings of
processes across scales are important for the global dynamics and
thermodynamics of the solar wind. We describe methods to measure in-situ
properties of particles and fields. We then discuss the role of expansion
effects, non-equilibrium distribution functions, collisions, waves and
turbulence, and kinetic microinstabilities for the multi-scale plasma
evolution.
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