Solar coronal heating: role of kinetic and inertial Alfvén waves in heating and charged particle acceleration

ABSTRACT A comprehensive understanding of solar coronal heating and charged particle acceleration remains one of the most critical challenges in space and astrophysical plasma physics. In this study, we explore the contribution of Alfvén waves – both in their kinetic (KAWs) and inertial (IAWs) regimes – to particle acceleration and solar coronal heating. Employing a kinetic plasma framework in the generalized Vlasov–Maxwell model, we analyse the dynamics of these waves with a focus on the perpendicular (i.e. across the magnetic field lines) Poynting flux vectors and the net resonant speed of the particles. We found the Poynting flux of KAWs decays rapidly, indicating short-range energy transport, while IAWs exhibit slower decay, enabling energy transfer over larger distances (R$_{\text{Sun}}$) in the solar corona. We also evaluate the electric potentials associated with KAWs and IAWs and find the KAW’s potentials are significantly enhanced at larger wavenumbers ($k_x \rho _i>0.1$) regimes, while IAWs exhibit reduced parallel and enhanced perpendicular electric potentials, governed by the perturbed electric fields (${E_x}$ and ${E_z}$) values. Additionally, we determine the net resonant speed of particles in the perpendicular direction and demonstrate that these wave–particle interactions can efficiently heat the solar corona over extended distances R$_{\text{Sun}}$. Finally, we quantify the power transported by KAWs and IAWs through solar flux loop tubes, finding that both wave types deliver greater energy with increasing ${T_e/T_i}$ and $c k_x/\omega _{pe}$ values. These insights not only deepen our theoretical understanding of wave-driven heating mechanisms but also provide valuable implications for interpreting solar wind, corona, heliospheric, and magnetospheric dynamics.