  We use 62 electron density profiles collected by the Radio Occultation
Science Experiment (ROSE), on MAVEN, when Mars was hit by CIRs and ICMEs close
to aphelion (April 2021) and during two dust storms (June-July 2022) to examine
the response of the Martian ionosphere to solar events and to solar events
hitting during dust storms. We do so through three proxies - variation in total
electron content between 80 and 300 km altitude, peak density, and peak
altitude - of the aforementioned 62 ROSE electron density profiles, relative to
a characterisation of the ionosphere through solar minimum leading to solar
maximum, specific to local time sector and season, presented in Segale et al.,
(COMPANION). We observe an increased Total Electron Content (TEC) between 80
and 300 km altitude up to 2.5 x 10(15) m(-2) in April 2021 and up to 5 x 10(15)
m(-2) in June-July 2022 compared to the baseline photochemically produced
ionosphere. This increase in TEC corresponds mainly to increases in the solar
energetic particles flux (detected by MAVEN SEP) and electron fluxes (detected
by MAVEN SWEA). In addition to solar events, in June-July 2022, an A storm and
a B storm were occurring and merging on the surface of Mars. We observe a raise
in peak altitude in general lower than expected during dust storms, possibly
due to high values of solar wind dynamic pressure (derived from MAVEN SWIA).
From 31 ROSE profiles collected in this time period that showed both the M2 and
M1 layer, we observe that, on average, M1 and M2 peak altitudes raise the same
amount, suggesting that the thermosphere might loft as a unit during dust
storms. During this time period, several proton aurora events of variable
brightness were detected with MAVEN IUVS underlining the complex and
multifaceted impact of dust activity and extreme solar activity on the Martian
ionosphere.
