Properties of ubiquitous magnetic reconnection events in the lower solar atmosphere

TL;DR

This study provides a comprehensive statistical analysis of quiet Sun Ellerman bombs, revealing their widespread occurrence, characteristics, and association with magnetic fields, supporting the reconnection along vertical current sheets.

Contribution

It offers the first extensive statistical characterization of QSEBs in the quiet Sun using high-resolution H$eta$ observations, detailing their properties and distribution.

Findings

2809 QSEBs detected in 1 hour of observations.

Median lifetime of QSEBs is 1.14 minutes.

QSEBs are more frequent near magnetic network regions.

Abstract

Magnetic reconnection in the deep solar atmosphere can give rise to enhanced emission in the Balmer hydrogen lines, a phenomenon referred to as Ellerman bombs. Recent high quality H$\beta$ observations indicate that Ellerman bombs are more common than previously thought and it was estimated that at any time about half a million Ellerman bombs are present in the quiet Sun. We performed an extensive statistical characterization of the quiet Sun Ellerman bombs (QSEBs) in these new H$\beta$ observations. We analyzed a 1 h dataset of quiet Sun observed with the Swedish 1-m Solar Telescope that consists of spectral imaging in the H$\beta$ and H$\alpha$ lines, as well as spectropolarimetric imaging in Fe I 617.3 nm. We detected a total of 2809 QSEBs. The lifetime varies between 9 s and 20.5 min with a median of 1.14 min. The maximum area ranges between 0.0016 and 0.2603 Mm$^2$ with a median of 0.018 Mm$^2$. A subset (14%) of the QSEBs display enhancement of the H$\beta$ line core. On average, the line core brightening appears 0.88 min after the onset of brightening in the wings, and the distance between these brightenings is 243 km. This gives rise to an apparent propagation speed ranging between $-$14.3 and +23.5 km s$^{-1}$, with an average that is upward propagating at +4.4 km $^{-1}$. The average orientation is nearly parallel to the limbward direction. QSEBs are nearly uniformly distributed over the field of view but we find empty areas with the size of mesogranulation. QSEBs are located more frequent near the magnetic network where they are often bigger, longer lived and brighter. We conclude that QSEBs are ubiquitous in quiet Sun and appear everywhere except in areas of mesogranular size with weakest magnetic field ($B_{\rm{LOS}}\lesssim50$~G). Our observations support the interpretation of reconnection along vertically extended current sheets.