1. Twilight Mesospheric Clouds in Jezero as Observed by MEDA Radiation and Dust Sensor (RDS)
- Author
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Física aplicada I, Fisika aplikatua I, Toledo, Daniel, Gomez Martín, Laura, Apestigue, Victor, Arruego, Ignacio, Smith, Michael D., Munguira Ruiz, Asier, Martínez, Germán, Patel, Priyaben, Sánchez Lavega, Agustín María, Lemmon, Mark T., Tamppari, Leslie, Viúdez Moreiras, Daniel, Hueso Alonso, Ricardo, Vicente Retortillo, Álvaro, Newman, Claire E., Lorenz, Ralph D., Yela, Margarita, de la Torre Juárez, Manuel, Rodríguez Manfredi, José Antonio, Física aplicada I, Fisika aplikatua I, Toledo, Daniel, Gomez Martín, Laura, Apestigue, Victor, Arruego, Ignacio, Smith, Michael D., Munguira Ruiz, Asier, Martínez, Germán, Patel, Priyaben, Sánchez Lavega, Agustín María, Lemmon, Mark T., Tamppari, Leslie, Viúdez Moreiras, Daniel, Hueso Alonso, Ricardo, Vicente Retortillo, Álvaro, Newman, Claire E., Lorenz, Ralph D., Yela, Margarita, de la Torre Juárez, Manuel, and Rodríguez Manfredi, José Antonio
- Abstract
The Mars Environmental Dynamics Analyzer instrument, on board NASA's Mars 2020 Perseverance rover, includes a number of sensors to characterize the Martian atmosphere. One of these sensors is the Radiation and Dust Sensor (RDS) that measures the solar irradiance at different wavelengths and geometries. We analyzed the RDS observations made during twilight for the period between sol 71 and 492 of the mission (Ls 39°–262°, Mars Year 36) to characterize the clouds over the Perseverance rover site. Using the ratio between the irradiance at zenith at 450 and 750 nm, we inferred that the main constituent of the detected high-altitude aerosol layers was ice from Ls = 39°–150° (cloudy period), and dust from Ls 150°–262°. A total of 161 twilights were analyzed in the cloudy period using a radiative transfer code and we found: (a) signatures of clouds/hazes in the signals in 58% of the twilights; (b) most of the clouds had altitudes between 40 and 50 km, suggesting water ice composition, and had particle sizes between 0.6 and 2 µm; (c) the cloud activity at sunrise is slightly higher that at sunset, likely due to the differences in temperature; (d) the time period with more cloud detections and with the greatest cloud opacities is during Ls 120°–150°; and (e) a notable decrease in the cloud activity around aphelion, along with lower cloud altitudes and opacities. This decrease in cloud activity indicates lower concentrations of water vapor or cloud condensation nuclei (dust) around this period in the Martian mesosphere.
- Published
- 2023