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Ozone is an important radiative trace gas in the Earth's atmosphere. Thepresence of ozone can significantly influence the thermal structure of anatmosphere, and by this e.g. cloud formation. Photochemical studies suggestthat ozone can form in carbon dioxide-rich atmospheres. We investigate theeffect of ozone on the temperature structure of simulated early Martianatmospheres. With a 1D radiative-convective model, we calculatetemperature-pressure profiles for a 1 bar carbon dioxide atmosphere. Ozoneprofiles are fixed, parameterized profiles. We vary the location of the ozonelayer maximum and the concentration at this maximum. The maximum is placed atdifferent pressure levels in the upper and middle atmosphere (1-10 mbar).Results suggest that the impact of ozone on surface temperatures is relativelysmall. However, the planetary albedo significantly decreases at large ozoneconcentrations. Throughout the middle and upper atmospheres, temperaturesincrease upon introducing ozone due to strong UV absorption. This heating ofthe middle atmosphere strongly reduces the zone of carbon dioxide condensation,hence the potential formation of carbon dioxide clouds. For high ozoneconcentrations, the formation of carbon dioxide clouds is inhibited in theentire atmosphere. In addition, due to the heating of the middle atmosphere,the cold trap is located at increasingly higher pressures when increasingozone. This leads to wetter stratospheres hence might increase water loss rateson early Mars. However, increased stratospheric H2O would lead to more HOx,which could efficiently destroy ozone. This result emphasizes the need forconsistent climate-chemistry calculations to assess the feedback betweentemperature structure, water content and ozone chemistry. Furthermore,convection is inhibited at high ozone amounts, leading to a stably stratifiedatmosphere.

Effect of O3 on the atmospheric temperature structure of early Mars