Analysis of a spatially deconvolved solar pore

TL;DR

This study employs advanced spatial deconvolution and inversion techniques on Hinode/SP data to analyze the physical properties of a solar pore, revealing detailed magnetic and thermal structures without artefacts.

Contribution

It introduces a combined approach of spatial deconvolution and Stokes profile inversion to accurately characterize solar pores, ensuring no artefacts are introduced in the analysis.

Findings

Inner pore has temperature lower than surroundings

Magnetic field strength exceeds 2 kG and is unipolar

Downward motions occur at low photosphere below $ au=-1$

Abstract

Solar pores are active regions with large magnetic field strengths and apparent simple magnetic configurations. Their properties resemble the ones found for the sunspot umbra although pores do not show penumbra. Therefore, solar pores present themselves as an intriguing phenomenon that is not completely understood. We examine in this work a solar pore observed with Hinode/SP using two state of the art techniques. The first one is the spatial deconvolution of the spectropolarimetric data that allows removing the stray light contamination induced by the spatial point spread function of the telescope. The second one is the inversion of the Stokes profiles assuming local thermodynamic equilibrium that let us to infer the atmospheric physical parameters. After applying these techniques, we found that the spatial deconvolution method does not introduce artefacts, even at the edges of the magnetic structure, where large horizontal gradients are detected on the atmospheric parameters. Moreover, we also describe the physical properties of the magnetic structure at different heights finding that, in the inner part of the solar pore, the temperature is lower than outside, the magnetic field strength is larger than 2 kG and unipolar, and the LOS velocity is almost null. At neighbouring pixels, we found low magnetic field strengths of same polarity and strong downward motions that only occur at the low photosphere, below the continuum optical depth $\log \tau=-1$. Finally, we studied the spatial relation between different atmospheric parameters at different heights corroborating the physical properties described before.