2D radiative modelling of He I spectral lines formed in solar prominences

TL;DR

This paper introduces a new 2D radiative modelling approach for He I spectral lines in solar prominences, combining self-consistent radiation transfer and non-LTE statistical equilibrium, validated by high-resolution observations.

Contribution

The paper presents a novel 2D radiative modelling code for He I lines in solar prominences, integrating detailed atomic models and self-consistent radiation transfer.

Findings

Preliminary results show good agreement with high-resolution observations.

The modelling approach effectively captures the formation of He I lines in prominences.

The code provides a new tool for solar prominence spectral analysis.

Abstract

We present preliminary results of 2D radiative modelling of He I lines in solar prominences, using a new numerical code developed by us (Leger, Chevallier and Paletou 2007). It treats self-consistently the radiation transfer and the non-LTE statistical equilibrium of H and, in a second stage, the one of He using a detailed atomic model. Preliminary comparisons with new visible plus near-infrared observations made at high spectral resolution with THeMIS are very satisfactory.