Atmospheric Tides Near the Equator on Mars

Diurnal solar radiation forces global oscillations in pressure, temperature, and wind fields. They are called atmospheric or thermal tides and are additionally modified by topography, surface properties, and atmospheric absorber consentration. They propagate around the planet in periods that are integer fractions of a solar day and are only relevant in the upper atmosphere on Earth, but they represent a very large part of the atmospheric circulation on Mars. First two harmonic components (diurnal and semi-diurnal), with periods of 24 and 12 hr at the locations of InSight and Mars Science Laboratory (MSL) are represented here with the comparison to Mars Climate Database (MCD) predictions.

Both of these landers are located in the tropics, InSight on Elysium Planitia (4.5°N, 135.6°E) and MSL within the Gale Crater (4.6°S, 137.4°E). In this study, we utilized observations of the time period from Martian year (MY) 34 solar longitude (Ls) 296° to MY 36 Ls 53°. Diurnal amplitude was larger than semi-diurnal amplitude on both platforms and similar sensitivity to atmospheric dust content was found. However, the amplitude of the semi-diurnal component was smoother than the diurnal amplitude due to its sensitivity to global atmospheric dust content. One clear difference between the platforms was the average amplitude of the diurnal tide, which was 17 Pa for InSight and 33 Pa for MSL. Lateral hydrostatic adjustment flow, generated by the topography causes this difference since it increases the diurnal range of pressure within the Gale. Diurnal tide phase at the InSight was lower than that at the MSL, with averages of 03:39 and 04:25 LTST. In addition, MSL detected roughly contant diurnal tide phase, but InSight observed much more variation. Semi-diurnal phase pattern was very similar on both platforms.

Diurnal tide amplitude predicted by the MCD mimicked the observations quite well at both locations, except during MY 35 Ls 0°–180°. During that time, MCD amplitudes were lower than observed. This is very likely explained by the atmospheric dust conditions, due to the sensitivity of the diurnal tide to the local atmospheric dust loading. MCD dust optical depth was in good agreement with MSL observed optical depth during MY 35 Ls 180°–360°, but was lower than observed during MY 35 Ls 0°–180°. MCD semi-diurnal amplitudes mimicked the observations well throughout MY 35 due to its sensitivity to global atmospheric dust loading.