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Author Maneva, Yana G. ♦ Poedts, Stefaan ♦ Viñas, Adolfo ♦ Araneda, Jaime
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword PARTICLE ACCELERATORS ♦ CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ♦ ASTROPHYSICS ♦ COMPUTERIZED SIMULATION ♦ DISPERSION RELATIONS ♦ DISTRIBUTION FUNCTIONS ♦ HEAVY IONS ♦ INTERPLANETARY SPACE ♦ MONOCHROMATIC RADIATION ♦ MULTICHARGED IONS ♦ OXYGEN IONS ♦ PARAMETRIC INSTABILITIES ♦ PHASE SPACE ♦ PLASMA ♦ PLASMA HEATING ♦ PROTON BEAMS ♦ SOLAR CORONA ♦ SOLAR ELECTRONS ♦ SOLAR PROTONS ♦ SOLAR WIND
Abstract Minor ions in the fast solar wind are known to have higher temperatures and to flow faster than protons in the interplanetary space. In this study we combine previous research on parametric instability theory and 2.5D hybrid simulations to study the onset of preferential heating of Oxygen 5{sup +} ions by large-scale finite-amplitude Alfvén waves in the collisionless fast solar wind. We consider initially non-drifting isotropic multi-species plasma, consisting of isothermal massless fluid electrons, kinetic protons and kinetic Oxygen 5{sup +} ions. The external energy source for the plasma heating and energization are oblique monochromatic Alfvén-cyclotron waves. The waves have been created by rotating the direction of initial parallel pump, which is a solution of the multi-fluid plasma dispersion relation. We consider propagation angles θ ≤ 30°. The obliquely propagating Alfvén pump waves lead to strong diffusion in the ion phase space, resulting in highly anisotropic heavy ion velocity distribution functions and proton beams. We discuss the application of the model to the problems of preferential heating of minor ions in the solar corona and the fast solar wind.
ISSN 0094243X
Educational Use Research
Learning Resource Type Article
Publisher Date 2016-03-25
Publisher Place United States
Volume Number 1720
Issue Number 1


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