Connecting Atmospheric Properties and Synthetic Emission of Shock Waves Using 3D RMHD Simulations of Quiet Sun

Abstract

We analyze the evolution of shock waves in high-resolution 3D radiative MHD simulations of the quiet Sun and their synthetic emission characteristics. The simulations model the dynamics of a 12.8x12.8x15.2 Mm quiet-Sun region (including a 5.2 Mm layer of the upper convection zone and a 10 Mm atmosphere from the photosphere to corona) with an initially uniform vertical magnetic field of 10 G, naturally driven by convective flows. We synthesize the Mg II and C II spectral lines observed by the IRIS satellite and EUV emission observed by the SDO/AIA telescope. Synthetic observations are obtained using the RH1.5D radiative transfer code and temperature response functions at both the numerical and instrumental resolutions. We found that the Doppler velocity jumps of the C II 1334.5 A IRIS line and a relative enhancement of the emission in the 335 A SDO/AIA channel are the best proxies for the enthalpy deposited by shock waves into the corona (with Kendall's $\tau$ correlation coefficients of 0.59 and 0.38, respectively). The synthetic emission of the lines and extreme ultraviolet passbands are correlated with each other during the shock wave propagation. All studied shocks are mostly hydrodynamic (i.e., the magnetic energy carried by horizontal fields is $\le$2.6% of the enthalpy for all events) and have Mach numbers > 1.0-1.2 in the low corona. The study reveals the possibility of diagnosing energy transport by shock waves into the solar corona, as well as their other properties, by using IRIS and SDO/AIA sensing observations.

arXiv comment31 pages, 8 figures, 2 tables

References in corpus (27)

• The Interface Region Imaging Spectrograph (IRIS)
• The stellar atmosphere simulation code Bifrost
• Dynamic Hydrogen Ionization
• The formation of IRIS diagnostics II. The formation of the Mg II h&k lines in the solar atmosphere
• Approximations for radiative cooling and heating in the solar chromosphere
• A publicly available simulation of an enhanced network region of the Sun
• Spectropolarimetric investigation of the propagation of magnetoacoustic waves and shock formation in sunspot atmospheres
• High-resolution Observations of the Shock Wave Behavior for Sunspot Oscillations with the Interface Region Imaging Spectrograph
• RH 1.5D: a massively parallel code for multi-level radiative transfer with partial frequency redistribution and Zeeman polarisation
• The formation of IRIS diagnostics V. A quintessential model atom of C II and general formation properties of the C II lines at 133.5 nm
• Excitation of acoustic waves by vortices in the quiet Sun
• Forward modeling of emission in SDO/AIA passbands from dynamic 3D simulations
• The formation of IRIS diagnostics VI. The Diagnostic Potential of the C II Lines at 133.5 nm in the Solar Atmosphere
• Dynamics of Magnetized Vortex Tubes in the Solar Chromosphere
• Non-equilibrium calcium ionisation in the solar atmosphere
• Three-dimensional modeling of chromospheric spectral lines in a simulated active region
• The Formation of IRIS Diagnostics. VII. The Formation of the OI 135.56 nm Line in the Solar Atmosphere
• On the Active Region Bright Grains Observed in the Transition Region Imaging Channels of IRIS
• Hinode and IRIS observations of the magnetohydrodynamic waves propagating from the photosphere to the chromosphere in a sunspot
• Vortex Tubes of Turbulent Solar Convection
• Magnetohydrodynamic Non-linearities in Sunspot Atmospheres: Chromospheric Detections of Intermediate Shocks
• Realistic modeling of local dynamo processes on the Sun
• Using Realistic MHD Simulations for Modeling and Interpretation of Quiet-Sun Observations with the Solar Dynamics Observatory Helioseismic and Magnetic Imager
• Shock Heating Energy of Umbral Flashes Measured with Integral Field Unit Spectroscopy
• Statistical Study of Chromospheric Evaporation in Impulsive Phase of Solar Flares
• Simulations of Stellar Magnetoconvection using the Radiative MHD Code `StellarBox'
• Origin of Deep Acoustic Sources Associated with Solar Magnetic Structures

Cited by in corpus (1)

• First Observation of Chromospheric Waves in a Sunspot by DKIST/ViSP: The Anatomy of an Umbral Flash