The detection of upwardly propagating waves channelling energy from the chromosphere to the low corona

TL;DR

This study identifies upwardly propagating waves in a solar pore, observed with high-resolution data, revealing their potential role in heating the solar corona by channeling wave energy from the chromosphere.

Contribution

First observation of upwardly propagating waves in a solar pore, demonstrating their presence outside sunspots and their potential contribution to coronal heating.

Findings

UPWs travel at ~17 km/s horizontally

Vertical velocity of UPWs is ~42 km/s

Wave energy estimated at ~150 W/m²

Abstract

There have been ubiquitous observations of wave-like motions in the solar atmosphere for decades. Recent improvements to space- and ground-based observatories have allowed the focus to shift to smaller magnetic structures on the solar surface. In this paper, high-resolution ground-based data taken using the Swedish 1 m Solar Telescope is combined with co-spatial and co-temporal data from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) satellite to analyze running penumbral waves (RPWs). RPWs have always been thought to be radial wave propagation that occurs within sunspots. Recent research has suggested that they are in fact upwardly propagating field-aligned waves (UPWs). Here, RPWs within a solar pore are observed for the first time and are interpreted as UPWs due to the lack of a penumbra that is required to support RPWs. These UPWs are also observed co-spatially and co-temporally within several SDO/AIA elemental lines that sample the transition region and low corona. The observed UPWs are traveling at a horizontal velocity of around 17 +- 0.5 km s-1 and a minimum vertical velocity of 42 +- 21 km s-1. The estimated energy of the waves is around 150 W m-2, which is on the lower bound required to heat the quiet-Sun corona. This is a new, yet unconsidered source of wave energy within the solar chromosphere and low corona.