Ygopro 2 my card backs are question marks

Heating and Acceleration of Solar Wind Ions by Turbulent Wave Spectrum in Inhomogeneous Expanding Plasma The non-Maxwellian velocity distribution functions (VDFs) of the ions are modeled in the inhomogeneous solar wind plasma in the acceleration region close to the Sun.Г‚В«Г‚В less The results of the study provide the ion temperature anisotropy and drift velocity temporal evolution due to relaxation of the instability. The acceleration of the solar wind ions is achieved by the parametric instability of large amplitude waves in the spectrum, and is also affected by the inhomogeneity. It is found that the turbulent wave spectrum of initially parallel propagating waves cascades to oblique modes, and leads to enhanced resonant ion heating due to the inhomogeneity. The effect of super-AlfvГѓВ©nic ion drift on the ion heating is investigated. The effects ofmoreГ‚В Г‚В» background density inhomogeneity across the magnetic field on the resonant ion heating are studied. Turbulent magnetic fluctuations dominated by power-law frequency spectra, which are evident from in-situ as well as remote sensing measurements, are used in our models. The hybrid model describes the kinetics of the ions, while the electrons are modeled as massless neutralizing fluid in an expanding box approach. The heating and the acceleration of the solar wind ions by turbulent wave spectrum in inhomogeneous plasma is studied using a 2.5D hybrid model. Near the Sun (< 10R) the acceleration, heating, and propagation of the solar wind are likely affected by the background inhomogeneities of the magnetized plasma. Ofman, Leon, E-mail: NASA Goddard Space Flight Center, Greenbelt, MD Visiting, Department of Geosciences, Tel Aviv University, Tel Aviv Heating and acceleration of solar wind ions by turbulent wave spectrum in inhomogeneous expanding plasma The model parameters are applicable to the expected solar wind conditions at about 10 solar radii. It was found that the scaling of the magnetic fluctuations power spectrum steepens in the higher-density regions, and the heating is channeled to these regions from the surrounding lower-density plasma due to wave refraction. We investigate the parametric dependence of the perpendicular heating, and the temperature anisotropy in the H+-He++ solar wind plasma. The 2-D hybrid model treats parallel and oblique waves, together with cross-field inhomogeneity, self-consistently. We also investigate the effects of He++ ion beams in the inhomogeneous background plasma density on the heating of the solar wind plasma. This is the first two-dimensional hybrid parametric study of the solar wind plasma that includes an input turbulent wave spectrum guided by observation with inhomogeneous background density.

In the hybrid model the protons and heavy ions are treated kinetically as particles, while the electrons are included as neutralizing background fluid. We study the heating and the acceleration of multi-ion plasma in the solar wind by a turbulent spectrum of Alfvenic fluctuations using a 2-D hybrid numerical model. Remote sensing observations of the corona indicate that heavy ions are hotter than protons and their temperature is anisotropic (T(sub perpindicular / T(sub parallel) > 1). Observations of the solar wind plasma at 0.3 AU and beyond show that a turbulent spectrum of magnetic fluctuations is present. Hybrid Model of Inhomogeneous Solar Wind Plasma Heating by Alfven Wave Spectrum: Parametric Studies Also discussed are the structure of two-scale transport theories, and their relationship to WKB theory in light of multiple-scales analysis. Attention is given to the WKB formalism that has been used in many solar wind-related physics applications, with a view to its shortcomings. P.ДЄn evaluation is conducted of recent theories of small-scale MHD turbulence transport in an inhomogeneous background that are pertinent to the evolution of solar wind turbulence. Weakly inhomogeneous MHD turbulence and transport of solar wind fluctuations

Ygopro 2 my card backs are question marks