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We analyze the evolution of shock waves in high-resolution 3D radiative MHDsimulations of the quiet Sun and their synthetic emission characteristics. Thesimulations 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 atmospherefrom the photosphere to corona) with an initially uniform vertical magneticfield of 10 G, naturally driven by convective flows. We synthesize the Mg IIand C II spectral lines observed by the IRIS satellite and EUV emissionobserved by the SDO/AIA telescope. Synthetic observations are obtained usingthe RH1.5D radiative transfer code and temperature response functions at boththe numerical and instrumental resolutions. We found that the Doppler velocityjumps of the C II 1334.5 A IRIS line and a relative enhancement of the emissionin the 335 A SDO/AIA channel are the best proxies for the enthalpy deposited byshock waves into the corona (with Kendall's $\tau$ correlation coefficients of0.59 and 0.38, respectively). The synthetic emission of the lines and extremeultraviolet passbands are correlated with each other during the shock wavepropagation. All studied shocks are mostly hydrodynamic (i.e., the magneticenergy carried by horizontal fields is $\leq{}$2.6% of the enthalpy for allevents) and have Mach numbers > 1.0-1.2 in the low corona. The study revealsthe possibility of diagnosing energy transport by shock waves into the solarcorona, as well as their other properties, by using IRIS and SDO/AIA sensingobservations.

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