Numerical simulations of solar macrospicules

TL;DR

This paper uses numerical simulations with a realistic temperature model to show how velocity pulses in the chromosphere can trigger macrospicules, supported by observational case studies.

Contribution

It extends previous models by incorporating a VAL-C temperature profile and demonstrates macrospicule formation through velocity pulses in a 2D MHD framework.

Findings

Velocity pulses trigger plasma perturbations resembling macrospicules.

Numerical simulations align with observed macrospicule features.

Chromospheric velocity pulses can initiate macrospicule formation.

Abstract

Context. We consider a localized pulse in the component of velocity, parallel to the ambient magnetic field lines, that is initially launched in the solar chromosphere. Aims. We aim to generalize the recent numerical model of spicule formation (Murawski & Zaqarashvili 2010) by implementing a VAL-C model of solar temperature. Methods. With the use of the code FLASH we solve two-dimensional ideal magnetohydrodynamic equations numerically to simulate the solar macrospicules. Results. Our numerical results reveal that the pulse located below the transition region triggers plasma perturbations, which exhibit many features of macrospicules. We also present an observational (SDO/AIA 304 A) case study of the macrospicule that approximately mimics the numerical simulations. Conclusions. In the frame of the model we devised, the solar macrospicules can be triggered by velocity pulses launched from the chromosphere.