Diagnostics of the Prominence Plasma from H and Mg ii Spectral Observations

• Published in: The Astrophysical journal Vol. 886; no. 2
• Main Authors: Ruan, Guiping, Jej i, Sonja, Schmieder, Brigitte, Mein, Pierre, Mein, Nicole, Heinzel, Petr, Gunár, Stanislav, Chen, Yao
• Format: Journal Article
• Language: English
• Published: The American Astronomical Society 29.11.2019
• Subjects: radiative transfer; Sun: filaments, prominences; techniques: imaging spectroscopy
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ab4b50

The goal of this paper is to derive the physical conditions of the prominence observed on 2017 March 30. To do so, we use a unique set of data in Mg ii lines obtained with the space-borne Interface Region Imaging Spectrograph (IRIS) and in H line with the ground-based Multi-Channel Subtractive Double Pass spectrograph operating at the Meudon solar tower. Here, we analyze the prominence spectra of Mg ii h and k lines, and the H line in the part of the prominence which is visible in both sets of lines. We compute a grid of 1D NLTE (i.e., departures from the local thermodynamical equilibrium) models providing synthetic spectra of Mg ii k and h, and H lines in a large space of model input parameters (temperature, density, pressure, and microturbulent velocity). We compare Mg ii and H line profiles observed in 75 positions of the prominence with the synthetic profiles from the grid of models. These models allow us to compute the relationships between the integrated intensities and between the optical thickness in H and Mg ii k lines. The optical thickness τH is between 0.05 and 2, and is between 3 and 200. We show that the relationship of the observed integrated intensities agrees well with the synthetic integrated intensities for models with a higher microturbulence (16 km s−1) and T around 8000 K, ne = 1.5 × 1010 cm−3, p = 0.05 dyne. In this case, large microturbulence values could be a way to take into account the large mixed velocities existing in the observed prominence.