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WAVE ENERGY ON MARS AND EARTH: CONSIDERING LACUSTRINE EROSION

Introduction: Many researchers have identified lacustrine features on Mars[1]; this interpretation has important implications for the climate history of Mars and selection of future landing sites. It is, however, unclear if wave conditions on the Martian surface would be adequate to produce lacustrine features. Wave spectrums have been considered on Titan [2, 3], but not on Mars. This abstract outlines a quantitative assessment of wave energy available for lacustrine erosion on Mars and finds that time averaged wave energy on Mars might be similar to time averaged wave energy on Earth. Background: Shoreline erosion is a function of wave energy reaching the shore and the erodability of shoreline material. Wave energy is a function of wave height and period. The general wave equations predict expected wave behavior. The velocity of a wave scales with gravity while wave height scales with the inverse of gravity. Therefore, waves produced in the lower gravity of Mars can be expected to grow taller but travel slower. The energy of a wave is expressed by E=1/8rgH, where r is the fluid density (gm/cm), g is planetary gravity (m/s), and H is wave height (m). In order to estimate the amount of energy in the system over time, it is also important to know the wave period. Empirical equations have been developed for the earth to calculate significant wave height (hs), the average height of waves in the upper one-third of the wave energy spectrum, and the average frequency (fm) of the significant waves. The two empirical relations are the Pierson-Moskowitz(PM) equation, which is only a function of wind speed, and the JONSWAP equation which is a function of wind speed and fetch [4]. This abstract will use the PM equation, which assumes a fully developed sea [5]. The PM equation for significant wave height is: