Impact of Type II Spicules in the Corona: Simulations and Synthetic Observables

TL;DR

This study uses advanced 2.5D radiative MHD simulations to explore how type II spicules influence the solar corona, revealing their role in mass supply, wave propagation, and heating, aligning with recent observations.

Contribution

It introduces novel simulations including ion-neutral interactions to demonstrate the impact of type II spicules on coronal dynamics and heating, providing a comprehensive theoretical framework.

Findings

Type II spicules drive magneto-acoustic shocks and flows supplying mass to coronal loops.

Transversal magnetic waves and electric currents propagate at Alfvén speeds and dissipate, heating the corona.

Simulated spectral signatures match observed blue-shifted components and propagating disturbances in the corona.

Abstract

The role of type II spicules in the corona has been a much debated topic in recent years. This paper aims to shed light on the impact of type II spicules in the corona using novel 2.5D radiative MHD simulations including ion-neutral interaction effects with the Bifrost code. We find that the formation of simulated type II spicules, driven by the release of magnetic tension, impacts the corona in various manners. Associated with the formation of spicules, the corona exhibits 1) magneto-acoustic shocks and flows which supply mass to coronal loops, and 2) transversal magnetic waves and electric currents that propagate at Alfv\'en speeds. The transversal waves and electric currents, generated by the spicule's driver and lasting for many minutes, are dissipated and heat the associated loop. These complex interactions in the corona can be connected with blue shifted secondary components in coronal spectral lines (Red-Blue asymmetries) observed with Hinode/EIS and SOHO/SUMER, as well as the EUV counterpart of type II spicules and propagating coronal disturbances (PCDs) observed with the 171~\AA\ and 193~\AA\ SDO/AIA channels.