# The dark side of penumbral microjets: Observations in H\alpha

## TL;DR

This study observes penumbral microjets in multiple spectral lines, revealing their magnetic and dynamic properties, and suggests they are heat fronts propagating at the Alfvén velocity rather than typical jets.

## Contribution

First detailed multi-line observations of penumbral microjets showing their magnetic and velocity characteristics, proposing they are heat fronts rather than jets.

## Key findings

- PMJs are visible in H extalpha ext, appearing as dark features with LOS upflows.
- Average length and lifetime of PMJs are 2815 km and 163 seconds.
- PMJs exhibit POS velocities up to 17 km/s and increased LOS magnetic fields up to 100 G.

## Abstract

We present data of 10 penumbral microjets (PMJs) observed in H\alpha, Ca II 8542 \AA, and Fe I 6302 \AA line pair with the Swedish 1 m Solar Telescope (SST) with CRISP and Ca II K with SST/CHROMIS in active region NOAA 12599 on the 12th October 2016 at \mu=0.68. All four Stokes parameters of the Ca II 8542 \AA and Fe I 6302 \AA lines were observed and a series of test pixels was inverted using the Stockholm inversion code. Our analysis revealed for the first time that PMJs are visible in H\alpha, where they appear as dark features with average line-of-sight (LOS) upflows of 1.1\pm0.6 km/s, matching the LOS velocities from the inversions. Based on the H\alpha observations we extend the previous average length and lifetime of PMJs to 2815\pm530 km and 163\pm25 s, respectively. The plane-of-sky (POS) velocities of our PMJs of up to 17 km/s tend to give increased velocities with distance travelled. Furthermore, two of our PMJs with significant Stokes V signal indicate that the PMJs possess an increased LOS magnetic field of up to 100 G compared to the local pre-/post- PMJ magnetic field, which propagates as quickly as the PMJs' POS velocities. Finally, we present evidence that PMJs display an on average 1 minute gradual precursory brightening that only manifests itself in the cores of the Ca II lines. We conclude that PMJs are not ordinary jets but likely are manifestations of heat fronts that propagate at the local Alfven velocity.