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Is the Martian ionosphere symmetric in local time? Does the ionosphere changebetween aphelion, when there is no dust in the atmosphere, compared toperihelion, when the temperature rises and there is dust in the air even if nostorm is blowing? We utilize data from the MAVEN Radio Occultation ScienceExperiment (Withers et al., 2020) - with unprecedented coverage in solar zenithangle - to answer these questions and isolate the effects that local time andseason induce on the ionosphere at solar minimum. 219 out of the 1228 electrondensity profiles of the Martian ionosphere collected by MAVEN ROSE between July2016 and December 2022 show, besides the ever-present dayside M2 layer, adistinct M1 layer right below. This allowed us to study the behavior of the M2and M1 peak density and altitude as a function of solar zenith angle, and,also, for the first time, local time, and Martian season. We find that the M1layer at low SZA can occur at altitudes lower than 100 km; that the peakaltitudes and densities of both the M2 and M1 layers change more with seasonthan at the dusk ionosphere; and that the M2 peak density decreases at a fasterrate than the M1 with SZA. This study provides a baseline to accuratelycharacterize the photoproduced Martian ionosphere at solar minimum.

Characterization of the M1 and M2 layers in the undisturbed Martian ionosphere at solar minimum with MAVEN ROSE