Thermodynamic Properties of the Evershed Flow in the Lower Chromosphere

TL;DR

This study investigates the thermodynamic properties of the inverse Evershed flow in sunspot fibrils using spectropolarimetric data, revealing flow angles, temperature enhancements, and supporting the siphon flow model with shock features.

Contribution

It provides detailed thermodynamic and flow angle measurements of the inverse Evershed flow, confirming the siphon flow model with shock features in the chromosphere.

Findings

Flow velocities decrease from 3-15 km/s to zero at fibril footpoints.

Fibrils are inclined 30-60 degrees to the vertical.

Temperature increases by up to 2000K in the chromosphere.

Abstract

We used spectropolarimetric observations of a sunspot in active region NOAA 11809 in the Ca ii line at 854.2 nm taken with the SpectroPolarimeter for Optical and Infrared Regions (SPINOR) at the Dunn Solar Telescope to infer thermodynamic parameters along one hundred super-penumbral fibrils that harbor the inverse Evershed flow. The fibrils were identified in line-of-sight (LOS) velocity and line core intensity maps and were located in a segment of the sunspot that showed a regular penumbra in the photosphere. The chromospheric LOS velocity abruptly decreases from 3 to 15 km/s to zero at the inner footpoints of the fibrils that are located from the mid penumbra to about 1.4 spot radii. The spectra often show multiple components, i.e., one at the rest wavelength and one with a strong red shift, which indicates spatially or vertically unresolved structures. The line-core intensity always peaks slightly closer to the umbra than the LOS velocity. An inversion of the spectra with the CAlcium Inversion using a Spectral ARchive (CAISAR) code provided us with temperature stratifications that allowed us to trace individual fibrils through the atmosphere and to determine the angle of the flows relative to the surface without any additional assumptions on the flow topology such as radial symmetry. We find that the fibrils are not horizontal near the downflow points, but make an angle of 30 to 60 degrees to the local vertical. The temperature is enhanced by 200K at log(tau) ~ -2 and up to 2000K at log(tau) ~ -6 over that of the quiet Sun, whereas there is no signature in the low photosphere. Our results are consistent with a critical, i.e., sonic, or super-sonic siphon flow along super-penumbral flux tubes in which accelerating plasma abruptly attains sub-critical velocity through a standing shock in or near the penumbra as predicted by Montesinos & Thomas (1993).