The solar atmosphere is composed of many species, which are populated at different
ionization and excitation levels. The upper chromosphere, transition region, and corona are …

Two scenarios of possible ion heating due to finite amplitude parallel propagating Alfvén
waves in the solar atmosphere are investigated using a one-dimensional test particle …

We present multicomponent solar wind models self-consistently incorporating the
contribution from dissipationless, monochromatic, hydromagnetic (with angular frequencies …

We study a kinetic excitation mechanism for high-frequency dispersive Alfvén waves in the
solar corona by magnetic reconnection events. The ion-cyclotron and Cerenkov kinetic …

This Letter describes a new phenomenon on the Parker Solar Probe of recurring plasma
density enhancements that have Δn/n∼ 10% and that occur at a repetition rate of∼ 5 Hz …

Alfvén waves are a particular class of magnetohydrodynamic waves relevant in many
astrophysical and laboratory plasmas. In partially ionized plasmas the dynamics of Alfvén …

Ion stochastic heating by a monochromatic Alfvén wave, which propagates obliquely to the
background magnetic field, has been studied by Chen et al. It is shown that ions can be …

The effect of inhomogeneous velocity flow on Alfvén wave dynamics in the solar wind is
investigated. Unlike existing studies in this field that model energy deposition from high …

In the parts of the solar corona and solar wind that experience the fewest Coulomb
collisions, the component proton, electron, and heavy ion populations are not in thermal …

Ion heating by Alfvén waves has been considered for long as the mechanism explaining
why the solar corona has a temperature several orders of magnitude higher than the …