Recent observations of CH₄ in the Martian atmosphere suggest that CH₄ has been added relatively recently. Several mechanisms for recent CH₄ release have been proposed including subsurface biological methanogenesis, abiogenic hydrothermal and/or volcanic activity, dissociation of CH₄ hydrates, atmospheric photolysis, or addition of organics via bolide impact. This study examines the effects of increasing salinity on gas hydrate stability and compares estimates of the Martian geothermal gradient to CH₄ and CO₂ hydrate stability fields in the presence of high salinity brines. The results demonstrate that salinity increases alone result in a significant decrease in the predicted hydrate stability zone within the Martian subsurface and may be a driving force in CH₄ hydrate destabilization. Active thermal and/or pressure fluctuations are not required in order for CH₄ hydrates to be the source of atmospheric CH₄.