Formation of solar spicules due to high-frequency perturbation in the solar photosphere

Abstract

Spicules are jet-like structures, visible on the Sun and noticed quite frequently during space-based observations of the solar chromosphere. It is important to understand the physical processes that could lead to the formation of taller spicules having heights larger than 6 Mm. In the present work, we have provided high-frequency photospheric perturbation and studied nonlinear processes in the spicule formation under the framework of magnetohydrodynamics (MHD). Perturbations in the solar photosphere include pressure perturbations and torsional velocity perturbations. The solar spicules in our model are formed due to the interaction of nonlinear MHD waves, specifically slow magneto-acoustic and Alfvén waves with the solar transition region. Through a self-consistent approach and 1.5D MHD simulations, we found that the high-frequency perturbation in the solar photosphere could generate taller spicules if a suitable wave period and height of the solar transition region are considered initially. The simulations are performed over a long time (e.g., up to 800 min), and in certain conditions, we found that the spicule reaches a height of 10 Mm and beyond. Furthermore, high-frequency perturbations play a significant role in forming the spicules and chromospheric heating. © 2025 COSPAR