Insights into Mercurys tidal stresses: Linking present and past potentials

A planets orbital eccentricity can experience major changes over time as a result of planetary secular perturbations. Mercury's proximity to the Sun, its unique 3:2 spin-orbit resonance, and its high orbital eccentricity makes it an intriguing subject for investigating tidal forces and their resulting stresses. Throughout its history, Mercury may have experienced a state of further heightened eccentricity, potentially leading to tidal forces significant enough to modify the planet's surface. In the study presented here, we explore the tidal potential currently influencing Mercury and examine possible historical values of eccentricity to estimate past stress values. Employing a four-layer crustal model, we calculate Love numbers that reflect Mercury's internal physical properties and compute global tidal potential, surface stresses, and radial tidal displacement with respect to location and position in orbit. A suggested past orbital eccentricity of e = 0.41 could produce estimated maximum principal surface stresses of ~ +/-70 kPa which are comparable to current diurnal tidal principal stress values for Europa and Enceladus (~ +/-85 kPa). At present, Mercury experiences tidal stress values of up to ~ +/-15 kPa with a tidal bulge that can radially displace the surface by a mean of ~ 2.3 m. As tidal stresses could have been significantly higher in the past, we can hypothesize that Mercury might have experienced surface alterations induced by its orbital dynamics. On the other hand, the present-day surface of the planet has not retained evidence of any tidal stress modifications, suggesting that these characteristics, if present, would have been likely covered by the volcanic activity that persisted up to 3 billion years ago. Sophisticated instruments like the BepiColombo Laser Altimeter (BELA), to be inserted into orbit around Mercury in early 2026 onboard the European Space Agencys BepiColombo mission, promise to provide unprecedented data and will be instrumental in precisely measuring Mercury's global topography, contributing to a more accurate understanding of the planet's surface variations. This, in turn, will aid in refining our calculations and representations of Mercury's internal structure and its evolution.