Solar Flare Arcade Modelling: Bridging the gap from 1D to 3D Simulations of Optically Thin Radiation

Abstract

Solar flares are 3D phenomenon but modelling a flare in 3D, including many of the important processes in the chromosphere, is a computational challenge. Accurately modelling the chromosphere is important, even if the transition region and corona are the areas of interest, due to the flow of energy, mass, and radiation through the interconnected layers. We present a solar flare arcade model, that aims to bridge the gap between 1D and 3D modelling. Our approach is limited to the synthesis of optically thin emission. Using observed active region loop structures in a 3D domain we graft simulated 1D flare atmospheres onto each loop, synthesise the emission and then project that emission onto to the 2D observational plane. Emission from SDO/AIA, GOES/XRS, and IRIS/SG Fe XXI 1354.1A was forward modelled. We analyse the temperatures, durations, mass flows, and line widths associated with the flare, finding qualitative agreement but certain quantitative differences. Compared to observations, the Doppler shifts are of similar magnitude but decay too quickly. They are not as ordered, containing a larger amount of scatter compared to observations. The duration of gradual phase emission from GOES and AIA emission is also too short. Fe XXI lines are broadened, but not sufficiently. These findings suggest that additional physics is required in our model. The arcade model that we show here as a proof-of-concept can be extended to investigate other lines and global aspects of solar flares, providing a means to better test the coronal response to models of flare energy injection.

arXiv commentAccepted for publication in the Astrophysical Journal, 22 pages, 18 figures

References in corpus (59)

• The chemical composition of the Sun
• The Interface Region Imaging Spectrograph (IRIS)
• An Observational Overview of Solar Flares
• CHIANTI - An atomic database for Emission Lines. Version 8
• Radiative Hydrodynamic Models of the Optical and Ultraviolet Emission from Solar Flares
• Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares
• Observing the Roots of Solar Coronal Heating - in the Chromosphere
• Dynamic Hydrogen Ionization
• A Unified Computational Model for Solar and Stellar Flares
• Deducing Electron Properties From Hard X-Ray Observations
• Temporal evolution of multiple evaporating ribbon sources in a solar flare
• The influence of numerical resolution on coronal density in hydrodynamic models of impulsive heating
• Temporal evolution of chromospheric evaporation: case studies of the M1.1 flare on 2014 September 6 and X1.6 flare on 2014 September 10
• Imaging and spectroscopic observations of magnetic reconnection and chromospheric evaporation in a solar flare
• Two components of the coronal emission revealed by EUV spectroscopic observations
• Evolution of reconnection along an arcade of magnetic loops
• The Atmospheric Response to High Nonthermal Electron Beam Fluxes in Solar Flares I: Modeling the Brightest NUV Footpoints in the X1 Solar Flare of 2014 March 29
• New Insights into White-Light Flare Emission from Radiative-Hydrodynamic Modeling of a Chromospheric Condensation
• Soft X-ray Pulsations in Solar Flares
• Simulations of the Mg II k and Ca II 8542 lines from an Alfvén Wave-heated flare chromosphere
• The 2014 March 29 X-flare: sub-arcsecond resolution observations of Fe XXI 1354.1
• Simultaneous IRIS and Hinode/EIS observations and modelling of the 27 October 2014 X 2.0 class flare
• Spatially-Resolved Nonthermal Line Broadening During The Impulsive Phase of a Solar Flare
• The Thermal Properties of Solar Flares Over Three Solar Cycles Using GOES X-ray Observations
• Spectral signatures of chromospheric condensation in a major solar flare
• Measurements of Absolute Abundances in Solar Flares
• Alfvénic Wave Heating of the Upper Chromosphere in Flares
• The Width Distribution of Loops and Strands in the Solar Corona -- Are we Hitting Rock Bottom ?
• Non-Equilibrium Processes in the Solar Corona, Transition Region, Flares, and Solar Wind \textit{(Invited Review)}
• Investigating the response of loop plasma to nanoflare heating using RADYN simulations
• Si IV Resonance Line Emission During Solar Flares: Non-LTE, Non-equilibrium, Radiation Transfer Simulations
• Elongation of Flare Ribbons
• Extreme Ultra-Violet Spectroscopy of the Lower Solar Atmosphere During Solar Flares
• Response of optical hydrogen lines to beam heating: I. Electron beams
• Decay Phase Cooling and Inferred Heating of M- and X-class Solar Flares
• Solar Flare Element Abundances from the Solar Assembly for X-rays (SAX) on MESSENGER
• Properties of chromospheric evaporation and plasma dynamics of a solar flare from IRIS observations
• Modeling Mg II h, k and Triplet Lines at Solar Flare Ribbons
• A Hydrodynamic Model of Alfvénic Wave Heating in a Coronal Loop and its Chromospheric Footpoints
• Nonlinear Force-Free Magnetic Field Fitting to Coronal Loops with and without Stereoscopy
• The Vertical Current Approximation Nonlinear Force-Free Field Code - Description, Performance Tests, and Measurements of Magnetic Energies Dissipated in Solar Flares
• Long Duration Flare Emission: Impulsive or Gradual Heating?
• Transition Region and Chromospheric Signatures of Impulsive Heating Events. II. Modeling
• On the sensitivity of the GOES flare classification to properties of the electron beam in the thick target model
• The Compatibility of Flare Temperatures Observed with AIA, GOES, and RHESSI
• Hard X-ray and UV Observations of the 2005 January 15 Two-ribbon Flare
• Reproducing Type II White-Light Solar Flare Observations with Electron and Proton Beam Simulations
• Two-Phase Heating in Flaring Loops
• The direct relation between the duration of magnetic reconnection and the evolution of GOES light curves in solar flares
• Modelling Of The Hydrogen Lyman Lines In Solar Flares
• Modelling Mg II During Solar Flares. I. Partial Frequency Redistribution, Opacity, and Coronal Irradiation
• The Duration of Energy Deposition on Unresolved Flaring Loops in the Solar Corona
• The Solar Flare Iron Abundance
• Chromospheric Nanoflares as a Source of Coronal Plasma: II. Repeating Nanoflares
• Efficient Calculation of Non-Local Thermodynamic Equilibrium Effects in Multithreaded Hydrodynamic Simulations of Solar Flares
• X-ray Source Heights in a Solar Flare: Thick-target versus Thermal Conduction Front Heating
• Modeling Mg II during Solar Flares. II. Non-equilibrium Effects
• Statistical Properties of Soft X-ray emission of solar flares
• A 3D Model of AR 11726 Heated by Nanoflares

Cited by in corpus (14)

• Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE): II. Flares and Eruptions
• He I 10830 Å Dimming During Solar Flares, I. The Crucial Role of Non-Thermal Collisional Ionisations
• The Neupert Effect of Flare UltraViolet and Soft X-ray Emissions
• Prospects of Detecting Non-thermal Protons in Solar Flares via Lyman Line Spectroscopy: Revisiting the Orrall-Zirker Effect
• Flare Induced Photospheric Velocity Diagnostics
• Spectral variations within solar flare ribbons
• A Model for Gradual Phase Heating Driven by MHD Turbulence in Solar Flares
• An approximate recipe of chromospheric radiative losses for solar flares
• Call and Response: A Time-Resolved Study of Chromospheric Evaporation in a Large Solar Flare
• Formation Of The Lyman Continuum During Solar Flares
• The Transition Region of Solar Flare Loops
• Next-Generation Comprehensive Data-Driven Models of Solar Eruptive Events
• A new view of the solar interface region from the Interface Region Imaging Spectrograph (IRIS)
• Solar Flare Heating with Turbulent Suppression of Thermal Conduction