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Observations at millimetre wavelengths provide a valuable tool to study thesmall scale dynamics in the solar chromosphere. We evaluate the physicalconditions of the atmosphere in the presence of a propagating shock wave andlink that to the observable signatures in mm-wavelength radiation, providingvaluable insights into the underlying physics of mm-wavelength observations. Arealistic numerical simulation from the 3D radiative Magnetohydrodynamic (MHD)code Bifrost is used to interpret changes in the atmosphere caused by shockwave propagation. High-cadence (1 s) time series of brightness temperature(T$_\text{b}$) maps are calculated with the Advanced Radiative Transfer (ART)code at the wavelengths $1.309$ mm and $1.204$ mm, which represents oppositesides of spectral band~$6$ of the Atacama Large Millimeter/submillimeter Array(ALMA). An example of shock wave propagation is presented. The brightnesstemperatures show a strong shock wave signature with large variation information height between $\sim0.7$ to $1.4$ Mm. The results demonstrate thatmillimetre brightness temperatures efficiently track upwardly propagating shockwaves in the middle chromosphere. In addition, we show that the gradient of thebrightness temperature between wavelengths within ALMA band $6$ can potentiallybe utilised as a diagnostics tool in understanding the small-scale dynamics atthe sampled layers.

philosophical transactions - royal society. mathematical, physical and engineering sciences/philosophical transactions - royal society. mathematical, physical and engineering sciences

Characterisation of shock wave signatures at millimetre wavelengths from Bifrost simulations