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This book consists of a selection of original papers of the leading scientists in the fields of Space and Planetary Physics, Solar and Space Plasma Physics with important contributions to the theory, modeling and experimental techniques of the solar wind exploration. Its purpose is to provide the means for interested readers to become familiar with the current knowledge of the solar wind formation and elemental composition, the interplanetary dynamical evolution and acceleration of the charged plasma particles, and the guiding magnetic field that connects to the magnetospheric field lines and adjusts the effects of the solar wind on Earth. I am convinced that most of the research scientists actively working in these fields will find in this book many new and interesting ideas.

Solar wind. --- Plasma, Solar --- Solar plasma --- Wind, Solar --- Solar activity --- Stellar winds --- Heliosphere (Astrophysics) --- Physical Sciences --- Engineering and Technology --- Earth and Planetary Sciences --- Astronomy and Astrophysics --- Space Physics

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This book presents recent results on the modelling of space plasmas with Kappa distributions and their interpretation. Hot and dilute space plasmas most often do not reach thermal equilibrium, their dynamics being essentially conditioned by the kinetic effects of plasma particles, i.e., electrons, protons, and heavier ions. Deviations from thermal equilibrium shown by these plasma particles are often described by Kappa distributions. Although well-known, these distributions are still controversial in achieving a statistical characterization and a physical interpretation of non-equilibrium plasmas. The results of the Kappa modelling presented here mark a significant progress with respect to all these aspects and open perspectives to understanding the high-resolution data collected by the new generation of telescopes and spacecraft missions. The book is directed to the large community of plasma astrophysics, including graduate students and specialists from associated disciplines, given the palette of the proposed topics reaching from applications to the solar atmosphere and the solar wind, via linear and quasilinear modelling of multi-species plasmas and waves within, to the fundamental physics of nonequilibrium plasmas.

Solar system --- Astrophysics --- Statistical physics --- zonnestelsel --- astrofysica --- statistiek --- fysica

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The orbital angular momentum states have been studied in the regime of Classical and Quantum Optics [1]. However, recently Mendonca et al. have predicted the theoretical foundations of intense Laser beam having orbital angular momentum state for Laser-Plasma interaction [2]. It exhibits paradigmatic alteration of Inverse Faraday's effect [3]. The orbital angular momentum states are being studied for plasma vortices [4]. In this regard, Kinetic theory developed for the orbital angular momentum states [5, 6] is based on Maxwellian distribution of the plasma constituents. However, most of the Space Plasmas and some of the Laboratory Plasmas exhibit non-thermal/non-Maxwellian behavior [7] due to spatial variation of number density, temperature, magnetic field intensity and background turbulence. In this regard, it would be very interesting if we can develop a kinetic theory that can help us in understanding the effect of orbital angular momentum part of the waves on these non-thermal plasma systems. In our research work we will develop a Kinetic Theory based model for studying non-Maxwellian/non-thermal plasmas in the presence of orbital angular momentum (OAM) states. We will use this theory to study the stability of plasma waves and vortices in the presence and absence of ambient magnetic field. For this purpose the Laguerre-Gaussian (LG) mode function will be employed to model the modified non-Maxwellian dielectric function for the study of wave particle interaction. The solutions will be obtained analytically and their validity will be verified by comparison with the numerical solution of the dispersion relation and stability parameter for the OAM oriented plasma modes. In our research work, we will present the non-Maxwellian/non-thermal OAM Kinetic Model using three dimensional Generalized Lorentzian/kappa (non-Maxwellian) distribution functions. The reason of selecting kappa or Generalized distribution function is its flexibility that we can also extract thermal effects for the large values of spectral indices. [1] J. D. Jackson, "Classical Electrodynamics", 2nd ed., Wiley New York ( 1962). [2] J. T. Mendonca, B. Thide and H. Then, "Stimulated Raman and Brillouin backscattering of collimated beams carrying orbital angular momentum", Phys. Rev. Lett. 102, 185005 (2009). [3] S. Ali, J. R. Davies and J. T. Mendonca,"Inverse Faraday effect with linearly polarized laser pulses", Phys. Rev. Lett. 105, 035001 (2010). [4] J. T. Mendonca, S. Ali and B. Thide,"Plasmons with orbital angular momentum", Phys. Plasmas 16, 112103 (2009). [5] J. T. Mendonca, "Kinetic description of electron plasma waves with orbital angular momentum",Phys. Plasmas 19, 112113 (2012). [6] S. A. Khan, Aman-ur-Rehman and J. T. Mendonca,"Kinetic study of ion-acoustic plasma vortices", Phys. Plasmas 21, 092109 (2014). [7] Kashif Arshad, Zahida Ehsan, S. A. Khan and S. Mahmood,"Solar wind driven dust acoustic instability with Lorentzian kappa distribution ", Phys. Plasmas 21, 023704 (2014).