Reversal-free CaIIH profiles: a challenge for solar chromosphere modeling in quiet inter-network

TL;DR

This study investigates the challenge of modeling reversal-free CaIIH profiles in the quiet solar chromosphere, revealing the existence of cool patches and conflicting with traditional hot or very cool chromosphere models.

Contribution

It demonstrates that current models with temperature rises cannot reproduce reversal-free profiles, indicating the need for revised chromospheric temperature structures.

Findings

Approximately 25% of observed profiles are reversal-free.

Models with temperature rises fail to match reversal-free profiles.

Cool patches exist in the chromospheric network, challenging existing models.

Abstract

We study chromospheric emission to understand the temperature stratification in the solar chromosphere. We observed the intensity profile of the CaIIH line in a quiet Sun region close to the disk center at the German Vacuum Tower Telescope. We analyze over 10^5 line profiles from inter-network regions. For comparison with the observed profiles, we synthesize spectra for a variety of model atmospheres with a non local thermodynamic equilibrium (NLTE) radiative transfer code. A fraction of about 25% of the observed CaIIH line profiles do not show a measurable emission peak in H_{2v} and H_{2r} wavelength bands (reversal-free). All of the chosen model atmospheres with a temperature rise fail to reproduce such profiles. On the other hand, the synthetic calcium profile of a model atmosphere that has a monotonic decline of the temperature with height shows a reversal-free profile that has much lower intensities than any observed line profile. The observed reversal-free profiles indicate the existence of cool patches in the interior of chromospheric network cells, at least for short time intervals. Our finding is not only in conflict with a full-time hot chromosphere, but also with a very cool chromosphere as found in some dynamic simulations.