# Observations of solar small-scale magnetic flux-sheet emergence

## TL;DR

This paper presents the first observational evidence of magnetic sheet emergence in the solar photosphere, revealing a new form of flux emergence characterized by horizontal magnetic fields and dynamic interactions with granules.

## Contribution

It provides the first clear observational characterization of magnetic sheet emergence, expanding understanding beyond the well-studied magnetic loops in solar magnetic flux emergence.

## Key findings

- Magnetic sheet emergence involves horizontal magnetic flux densities up to 194 Mx/cm$^{2}$.
- Emergence occurs within 10 minutes with fluxes around 10^{18} Mx.
- Magnetic flux interacts with convective motions, forming magnetic loops at granule edges.

## Abstract

Aims. Moreno-Insertis et al. (2018) recently discovered two types of flux emergence in their numerical simulations: magnetic loops and magnetic sheet emergence. Whereas magnetic loop emergence has been documented well in the last years, by utilising high-resolution full Stokes data from ground-based telescopes as well as satellites, magnetic sheet emergence is still an understudied process. We report here on the first clear observational evidence of a magnetic sheet emergence and characterise its development. Methods. Full Stokes spectra from the Hinode spectropolarimeter were inverted with the SIR code to obtain solar atmospheric parameters such as temperature, line-of-sight velocities and full magnetic field vector information. Results. We analyse a magnetic flux emergence event observed in the quiet-sun internetwork. After a large scale appearance of linear polarisation, a magnetic sheet with horizontal magnetic flux density of up to 194 Mx/cm$^{2}$ hovers in the low photosphere spanning a region of 2 to 3 arcsec. The magnetic field azimuth obtained through Stokes inversions clearly shows an organised structure of transversal magnetic flux density emerging. The granule below the magnetic flux-sheet tears the structure apart leaving the emerged flux to form several magnetic loops at the edges of the granule. Conclusions. A large amount of flux with strong horizontal magnetic fields surfaces through the interplay of buried magnetic flux and convective motions. The magnetic flux emerges within 10 minutes and we find a longitudinal magnetic flux at the foot points of the order of $\sim$$10^{18}$ Mx. This is one to two orders of magnitude larger than what has been reported for small-scale magnetic loops. The convective flows feed the newly emerged flux into the pre-existing magnetic population on a granular scale.