# Effects of ion-neutral collisions on AlfvÃ©n waves: The presence of forbidden zone and heavy damping zone

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We have presented the numerical simulation of the coupled equations governing the dynamics of kinetic AlfvÃ©n wave (KAW) and ion acoustic wave in the intermediateÎ² plasma, where Î² is the ratio of thermal pressure to the background magnetic pressure. We have also developed a simplified...

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Three types of processes, occurring in the weakly ionized plasmas of the Earthâ€™s ionosphere as well as in the solar chromosphere, are being compared with each other. The main objective is to elaborate on the differences introduced primarily by the grossly different magnitudes of the...

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Previous studies (e.g., Malara et al., Astrophys. J. 533, 523 (2000)) considered small-amplitude Alfven wave (AW) packets in Arnold-Beltrami-Childress (ABC) magnetic field using WKB approximation. They draw a distinction between 2D AW dissipation via phase mixing and 3D AW dissipation via...

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Nonlinear couplings among kinetic AlfvÃ©n waves are investigated for a three-component plasma consisting of electrons, protons, and heavy ions. The parametric instability is investigated, and the growth rate is obtained. In the kinetic regime, the growth rate for the parallel decay instability...

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In the present work, we have discussed the effects of adiabatic trapping of electrons on obliquely propagating AlfvÃ©n waves in a low Î² plasma. Using the two potential theory and employing the Sagdeev potential approach, we have investigated the existence of arbitrary amplitude coupled...

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The dispersion relation of Alfven waves have been theoretical studies by kinetic approaches. Dispersion relation of Alfven waves are measured in multi-component magnetosphere plasma consisting of mixture of hydrogen (H+), helium (He+) and Oxygen (O+) ions in magnetized cold plasma. The wave is...

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The effects of both density stratification and magnetic field expansion on torsional AlfvÃ©n waves in solar spicules are studied. Also, their eigenfrequencies, eigenfunctions, and the period ratio P/ P are obtained with a novel mathematical method. We showed that under some circumstances this...

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We analyze the oscillations of the H Î± profile width based on our observations of the chromosphere at the base of solar coronal holes. The maximum oscillation amplitude averaged over ten time series is 64 m 0 A. Direct calculations show that this value cannot be reached through temperature...

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The dynamical response of the solar corona to surface and sub-surface perturbations depends on the chromospheric stratification, and specifically on how efficiently these layers reflect or transmit incoming AlfvÃ©n waves. While it would be desirable to include the chromospheric layers in the...