# Hot prominence spicules launched from turbulent cool solar prominences

## TL;DR

This paper reports on the observation of turbulent, heated prominence spicules in solar filaments, revealing their role in mass transfer and filament decay through transition region dynamics.

## Contribution

It provides new observational evidence of turbulence-driven heating and spicule formation in solar prominences, enhancing understanding of filament evolution.

## Key findings

- Prominence spicules are generated by turbulence in filaments.
- Spicules are heated to at least 0.7 MK.
- Spicules contribute to filament evaporation and decay.

## Abstract

A solar filament is a dense cool condensation that is supported and thermally insulated by magnetic fields in the rarefied hot corona. Its evolution and stability, leading to either an eruption or disappearance, depend on its coupling with the surrounding hot corona through a thin transition region, where the temperature steeply rises. However, the heating and dynamics of this transition region remain elusive. We report extreme-ultraviolet observations of quiescent filaments from the Solar Dynamics Observatory that reveal prominence spicules propagating through the transition region of the filament-corona system. These thin needle-like jet features are generated and heated to at least 0.7 MK by turbulent motions of the material in the filament. We suggest that the prominence spicules continuously channel the heated mass into the corona and aid in the filament evaporation and decay. Our results shed light on the turbulence-driven heating in magnetized condensations that are commonly observed on the Sun and in the interstellar medium.