Spicule-like structures observed in 3D realistic MHD simulations

TL;DR

This study uses 3D MHD simulations to analyze features resembling type I solar spicules, revealing their dynamics, parameters, and potential driving mechanisms, with results comparable to solar observations.

Contribution

First detailed 3D MHD simulation analysis of type I spicule-like features incorporating realistic physics and magnetic flux emergence.

Findings

Simulated spicules show parabolic height-time profiles similar to observations.

Velocity and height ranges in simulations are narrower than in real data.

Shorter, slower spicules are associated with stronger ambient magnetic fields.

Abstract

We analyze features that resemble type i spicules in two different 3D numerical simulations in which we include horizontal magnetic flux emergence in a computational domain spanning the upper layers of the convection zone to the lower corona. The two simulations differ mainly in the preexisting ambient magnetic field strength and in the properties of the inserted flux tube. We use the Oslo Staggered Code (OSC) to solve the full MHD equations with non-grey and non-LTE radiative transfer and thermal conduction along the magnetic field lines. We find a multitude of features that show a spatiotemporal evolution that is similar to that observed in type i spicules, which are characterized by parabolic height vs. time profiles, and are dominated by rapid upward motion at speeds of 10-30 km/s, followed by downward motion at similar velocities. We measured the parameters of the parabolic profile of the spicules and find similar correlations between the parameters as those found in observations. The values for height (or length) and duration of the spicules found in the simulations are more limited in range than those in the observations. The spicules found in the simulation with higher preexisting ambient field have shorter length and smaller velocities. From the simulations, it appears that these kinds of spicules can, in principle, be driven by a variety of mechanisms that include p-modes, collapsing granules, magnetic energy release in the photosphere and lower chromosphere and convective buffeting of flux concentrations.