Two-horn quiescent prominence observed in Hα and Mg II h&k lines with THEMIS and IRIS^⋆

¹ ETH-Zurich, Hönggerberg campus, HIT building, Zürich, Switzerland
² PMOD/WRC, Dorfstrasse 33, 7260 Davos Dorf, Switzerland
e-mail: krzysztof.barczynski@pmodwrc.ch
³ LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris-Diderot, 5 place Jules Janssen, 92190 Meudon, France
⁴ SUPA School of Physics and Astronomy, The University of Glasgow, Glasgow G12 8QQ, UK
⁵ KU-Leuven, 3001 Leuven, Belgium
⁶ THEMIS, INSU, CNRS, UPS 3718 IAC, Via Lactea, 38200 La Laguna, Tenerife, Spain
⁷ University of Wrocław, Centre of Scientific Excellence – Solar and Stellar Activity, Kopernika 11, 51-622 Wrocław, Poland

Received: 22 January 2023
Accepted: 22 August 2023

Abstract

Context. Prominences are large magnetic structures in the corona filled by cool plasma with fast evolving fine structure.

Aims. We aim to better understand the plasma conditions in the fine structure of a quiescent prominence including two transient horns observed at the bottom of the cavity using the high resolution Interface Region Imaging Spectrograph (IRIS) and the MulTi-Raies (MTR) spectrograph of the Télescope Heliographique pour l’Etude du Magnétisme et des Instabilités Solaires (THEMIS) in the Canary Islands.

Methods. We analysed the spectra obtained in Hα by THEMIS and Mg II by IRIS and compare them with a grid of 23 940 1D radiative transfer models which include a prominence-to-corona transition region (PCTR). The full observed profiles of Mg II in each pixel are fitted completely by synthesised profiles with ×RMS (Cross RMS; an improved version of the rolling root mean square (rRMS) method). When the RMS is below a certain threshold value, we recover the plasma conditions from the parameters of the model best fitting the observed line profile. This criterion is met in two regions (the horns and edge of the prominence) where the line profiles can generally be described as single peaked.

Results. The 1D models suggest that two different kinds of model atmospheres correspond to these two regions. The region at the edge is found to be fitted mainly with isothermal and isobaric models, while the other area (the horns) is seen to be fitted with models with a PCTR that have optical thicknesses of less than 5. In the prominence edge, the theoretical relationship between the integrated intensities in Hα and Mg II is verified and corresponds to low emission measure values. In these regions the electron density is around 10¹⁰ cm⁻³, while it is one order of magnitude less in the horn regions around 10⁹ cm⁻³.

Conclusions. In the horns, we find some profiles are best fitted with models with high mean temperatures. This suggests that the hot PCTR found in the horns could be interpreted as prominence plasma in condensation phase at the bottom of the coronal cavity.