Atmospheric Tides Near the Equator on Mars

• DOI: 10.5194/egusphere-egu24-1333
• Publication Date: 2024-03-08T10:59:06Z
• Authors: Joonas Leino; Ari-Matti Harri; Don Banfield; Manuel de la Torr...; Mark Paton; Jose-Antonio Rodr...; Mark Lemmon; Hannu Savijärvi
• Keywords: Atmospheric tide

Diurnal solar radiation forces global oscillations in pressure, temperature, and wind fields. They are called atmospheric or thermal tides additionally modified by topography, surface properties, absorber consentration. propagate around the planet periods that integer fractions of a day only relevant upper atmosphere on Earth, but they represent very large part circulation Mars. First two harmonic components (diurnal semi-diurnal), with 24 12 hr at locations InSight Mars Science Laboratory (MSL) represented here comparison to Climate Database (MCD) predictions. Both these landers located tropics, Elysium Planitia (4.5°N, 135.6°E) MSL within Gale Crater (4.6°S, 137.4°E). In this study, we utilized observations time period from Martian year (MY) 34 longitude (Ls) 296° MY 36 Ls 53°. amplitude was larger than semi-diurnal both platforms similar sensitivity dust content found. However, component smoother diurnal due its content. One clear difference between average tide, which 17 Pa for 33 MSL. Lateral hydrostatic adjustment flow, generated topography causes since it increases range pressure Gale. tide phase lower MSL, averages 03:39 04:25 LTST. addition, detected roughly contant phase, observed much more variation. Semi-diurnal pattern platforms. predicted MCD mimicked quite well locations, except during 35 0°–180°. During time, amplitudes were observed. This is likely explained conditions, local loading. optical depth good agreement 180°–360°, throughout