Utilizing atmospheric temperature observed from Mars Years 33 to 36 by the Imaging Ultraviolet Spectrograph (IUVS) onboard the Mars Atmosphere and Volatile Evolution (MAVEN), we derive the diurnal and semidiurnal thermal tides from 90 to 160 km. The seasonal variations of diurnal (DW1) and semidiurnal (SW2) tides in the thermosphere and mesosphere, observed by the Mars Climate Sounder (MCS), along with vertical phase velocities, indicate different sources for the migrating tide in the lower and upper atmosphere. The seasonal variation of diurnal eastward wavenumber 2 (DE2) tide in the thermosphere corresponds well to its counterpart in the lower atmosphere. Vertical phase velocities indicate that the DE2 propagates upward from the lower atmosphere to ~150 km, except near the perihelion (solar longitude 210° to 270°). The upward propagation of this DE2 tide could potentially impact the vertical coupling between the Martian lower and upper atmosphere.

Utilizing atmospheric temperature observed from Mars Years 33 to 36 by the Imaging Ultraviolet Spectrograph (IUVS) onboard the Mars Atmosphere and Volatile Evolution (MAVEN) and Mars Climate Sounder (MCS) onboard Mars Reconnaissance Orbiter (MRO), we derive the diurnal and semidiurnal thermal tides from 30 to 160 km. Vertical phase velocities of the migrating tides indicate their upward propagation above 100 km during the dust season (solar longitude, Ls 240° to 300°). During the non-dust season (Ls 30° to 150°), the diurnal eastward wavenumber 2 (DE2) and wavenumber 3 (DE3) tides can propagate upward from the lower atmosphere to ~140 km. The seasonal variation of DE2 and DE3 amplitudes in the thermosphere corresponds well to their counterparts in the lower atmosphere, primarily controlled by their Hough (1,1) modes. The upward propagation of these tides could potentially impact the vertical coupling between the Martian lower and upper atmosphere.

High-frequency gravity waves (HFGWs) observed by the Zhurong/Tianwen-1 and Perseverance/Mars 2020 rovers between 09:00 and 11:00 local time, from Ls 140° to 165° in Mars Year 36 was investigated. By analyzing the eccentricity of hodographs for monochromatic wind perturbations obtained from harmonic fittings, HFGWs were identified via their predominantly linear characteristics. The background atmosphere stability was estimated using the Richardson number from the Dynamic Meteorology Laboratory general circulation model simulation. We find that the frequency of HFGWs doubled following the onset of a regional dust storm (RDS) in the Utopia Planitia region, where the Zhurong rover landed. The propagation directions of the HFGWs were determined using their polarization relationships. The HFGWs observed by Zhurong predominantly propagated north-south direction before the RDS and then east-west after. The propagation direction changes were likely due to the atmospheric instability changes in the region before and after the storm.