Abstract Details


Name: Sahel Dey
Affiliation: University of Newcastle Australia
Conference ID: TVS202510266
Title: The interplay of solar spicules and coronal swirling conduits: from 3D MHD models to observations
Authors and Co-Authors: Piyali Chatterjee, Robertus Erdélyi
Abstract Type: Invited by SOC
Abstract: Spicules are elongated plasma jets that are observed in the highly inhomogeneous and dynamic interface region between the visible solar surface and the million-kelvin hot solar corona. With high spatial and temporal resolution observations, it is frequently detected that bunches of spicules undergo a variety of complex dynamics, e.g., lateral swaying and bulk spinning motion. The swaying motion is well explained as the effect of the propagating Kink waves, but the mechanism behind the rapid spinning motion is still under debate. Here, we present our three-dimensional radiative magnetohydrodynamic (rMHD) model from the Pencil code, which covers a part of the sub-surface convection zone to the solar corona. Analyzing 3D data cubes, we report multiple examples of spinning bunches of synthetic spicules with a lifetime of 0.5-2 min and rotational speed of 2-20 km/s, similar to those detected in Hinode and IRIS observations. In the process of forward modelling, we uncover another characteristic of the spicule forest that manifests as a two-dimensional plasma sheet, instead of one-dimensional conical spikes. The spinning motion of spicules, according to our findings, is due to the interplay of these jet structures with hot swirling plasma columns, extending to coronal heights – which we term as coronal swirling conduits (CoSCo). Following their excitation process, we categorize CoSCos into two different classes and one of which is triggered in situ in the chromosphere. Several of these CoSCos can potentially form by feeding on spicules and further channel this energy to the solar corona to maintain the million-kelvin temperature. Finally, we conclude with a brief comparative study of mass and energy fluxes from several 3D MHD models and connect them with observational estimations.