Mesospheric clouds in Jezero as observed by MEDA Radiation and Dust Sensor (RDS) at twilight 

<p>Clouds on Mars are primary elements for understanding the past and present climate of the planet. Cloud particles can affect the energy balance of the planet, and so the atmospheric dynamic, as well as influence the vertical distribution of dust particles through dust scavenging. The dust scavenging by clouds has critical consequences in the water cycle of the planet; e.g. regions in the atmosphere with insufficient quantity of dust particles (or condensation nuclei) can inhibit the formation of H₂O clouds and thus lead to the presence of water vapor in excess of saturation. The study of these interactions requires observations whose analysis allows us to infer simultaneously the properties of both the clouds and dust. To address these observations, the Radiation and Dust Sensor (RDS) is part of the Mars Environmental Dynamics Analyzer (MEDA) payload onboard of the Mars 2020 rover Perseverance.</p> <p>In this work we analysed the RDS observations made during twilight in the period Ls 39^&#9702;-262^&#9702; to characterize the clouds above &#8764; 30 km over the Perseverance rover site. From the ratio between the irradiance measured at zenith at 450 nm and 750 nm, we inferred that from Ls= 39^&#9702; to 150^&#9702; (referred as the cloudy period), water ice is the main constituent of the detected high-altitude aerosol layers. For Ls 150^&#9702;-262^&#9702; dust is the main aerosol present. A total of 161 twilights were analysed in the cloudy period with a radiative transfer code in spherical geometry. Among other results we found: i) signatures of clouds or hazes on the RDS signals in the 58 % of the twilights; ii) most of the clouds were at altitudes between 40 km and 50 km and with particle sizes between 0.6 &#956;m and 2 &#956;m (in effective radius); iii) the cloud activity at sunrise is slightly higher that at sunset (65 % against 52 %), likely due to the differences in temperature; iv) the cloudiest time in Perseverance site and with the greatest cloud opacities is in Ls 120^&#9702;-150^&#9702;; and v) a notable decrease in the cloud activity around the aphelion (Ls &#8764; 70^&#9702;), along with lower cloud altitudes and opacities. The drop in cloud activity around Ls &#8764; 70^&#9702; indicates lower concentrations of water vapor or cloud nuclei (dust) around this period in the Martian mesosphere. In this presentation, we will discuss the implications of our results on the water cycle of the planet.</p>