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Thermal dissociation and recombination of molecular hydrogen, H_2, in theatmospheres of ultra-hot Jupiters (UHJs) has been shown to play an importantrole in global heat redistribution. This, in turn, significantly impacts theirplanetary emission, yet only limited investigations on the atmospheric effectshave so far been conducted. Here we investigate the heat redistribution causedby this dissociation/recombination reaction, alongside feedback mechanismsbetween the atmospheric chemistry and radiative transfer, for a planetary andstellar configuration typical of UHJs. To do this, we have developed atime-dependent pseudo-2D model, including a treatment of time-independentequilibrium chemical effects. As a result of the reaction heat redistribution,we find temperature changes of up to $\sim$400 K in the atmosphere. When TiOand VO are additionally considered as opacity sources, these changes intemperature increase to over $\sim$800 K in some areas. This heatredistribution is found to significantly shift the region of peak atmospherictemperature, or hotspot, towards the evening terminator in both cases. Theimpact of varying the longitudinal wind speed on the reaction heat distributionis also investigated. When excluding TiO/VO, increased wind speeds are shown toincrease the impact of the reaction heat redistribution up to a threshold windspeed. When including TiO/VO there is no apparent wind speed threshold, due tothermal stabilisation by these species. We also construct pseudo-2D phasecurves from our model, and highlight both significant spectral flux damping andincreased phase offset caused by the reaction heat redistribution.

Pseudo-2D Modelling of Heat Redistribution Through H$_2$ Thermal Dissociation/Recombination: Consequences for Ultra-Hot Jupiters