Evaluation of different recipes for chromospheric radiative losses in solar flares
arXiv:2210.04461 · doi:10.1051/0004-6361/202244615
Abstract
Context. Radiative losses are an indispensable part in the numerical simulation of flares. Detailed calculations could be computationally expensive, especially in the chromosphere. There have been some approximate recipes for chromospheric radiative losses in flares, yet their feasibility in flare simulations needs further evaluation. Aims. We aim to evaluate the performance of different recipes for chromospheric radiative losses in flare simulations. Methods. We compare the atmospheric structure and line profiles in beam-heated flares calculated with detailed radiative losses and the approximate recipes. Results. Both GF90 and HCD22 recipes provide acceptable total radiative losses compared with detailed one, but there are discrepancies in the different atmospheric layers during the different evolutionary phases, which leads to misestimations of temperature and line intensity. The recipe of GF90 overestimates the coolings in the upper chromosphere greatly when temperature exceeds 10^5 K, which also affects the flare evolution and line asymmetries. Radiative heating in the middle chromosphere only functions in the initial stage and could be safely neglected. However, radiative heating from Lyman continuum could dominate near the transition region.
arXiv comment16 pages, 11 figures, 3 tables. A&A accepted
References in corpus (29)
- The stellar atmosphere simulation code Bifrost
- Radiative Hydrodynamic Models of the Optical and Ultraviolet Emission from Solar Flares
- Does a Non-Magnetic Solar Chromosphere Exist?
- The formation of the Halpha line in the solar chromosphere
- Dynamic Hydrogen Ionization
- A Unified Computational Model for Solar and Stellar Flares
- Solar UV and X-Ray Spectral Diagnostics
- Approximations for radiative cooling and heating in the solar chromosphere
- STiC -- A multi-atom non-LTE PRD inversion code for full-Stokes solar observations
- Fast magnetic reconnection in the solar chromosphere mediated by the plasmoid instability
- The influence of numerical resolution on coronal density in hydrodynamic models of impulsive heating
- RH 1.5D: a massively parallel code for multi-level radiative transfer with partial frequency redistribution and Zeeman polarisation
- Non-LTE inversions of the Mg II h&k and UV triplet lines
- Transient small-scale brightenings in the quiet solar corona: a model for campfires observed with Solar Orbiter
- Heating mechanisms in the low solar atmosphere through magnetic reconnection in current sheets
- Si IV Resonance Line Emission During Solar Flares: Non-LTE, Non-equilibrium, Radiation Transfer Simulations
- Chromospheric Extension of the MURaM Code
- Response of optical hydrogen lines to beam heating: I. Electron beams
- A Magnetic Reconnection model for Hot Explosions in the Cool Atmosphere of the Sun
- Formation of the helium EUV resonance lines
- Numerical Simulations of Chromospheric Microflares
- Diagnostics of Ellerman Bombs with High-resolution Spectral Data
- Modeling Mg II during Solar Flares. II. Non-equilibrium Effects
- Can the temperature of Ellerman Bombs be more than 10000K?
- The Response of the Lyman-Alpha Line in Different Flare Heating Models
- Hydrogen Emission in Type II White-light Solar Flares
- An approximate recipe of chromospheric radiative losses for solar flares
- Fast magnetic wave could heat the solar low-beta chromosphere
- Radiative losses in the chromosphere during a C-class flare