The thermal impact of the self-heating effect on airless bodies. The case of Mercury’s north polar craters

Thermal models are essential for studying airless planetary surfaces, as the interaction between topography and thermophysical properties plays a crucial role in determining a surface’s response to localized illumination. Accurate temperature distribution calculations require a comprehensive investigation of sunlight scattering, a process that, despite its computational challenges, cannot be overlooked, especially when high resolution is necessary. Furthermore, thermal analysis is fundamental for assessing the stability of volatiles in polar regions. In this study, we introduce a novel approach by discretizing the Sun into 100 individual elements, allowing for a highly precise simulation of solar flux—an innovation crucial for accurately capturing temperature distributions in Mercury’s polar craters, given the planet’s proximity to the Sun. This level of discretization significantly enhances the accuracy of the thermal model, ensuring a more realistic depiction of how sunlight interacts with crater topography. We developed a dual-model approach that simulates both direct solar illumination and its scattering on two craters, Laxness and Fuller, located at Mercury’s north pole. The illumination and thermal model predict temperature distribution and heat transfer based on the material’s thermal properties and topography. The study examines the interaction between direct sunlight, causing localized heating, and scattered light, which influences the thermal response of surface materials. Detailed illumination maps and temperature profiles were generated over two Hermean years, revealing the significant impact of the self-heating effect on temperature distribution. The results show that specific regions experience indirect solar flux due to the craters’ morphology, particularly in permanently shadowed regions (PSRs) that are heated exclusively by scattered radiation. Maximum temperature profiles for the Laxness and Fuller craters show a substantial temperature increase within PSRs compared to areas exposed to direct illumination. However, while self-heating does not affect the stability of water ice in the Laxness crater, in the Fuller crater, a section within the radar-bright material reaches temperatures of up to 210 K, potentially threatening the stability of water ice. Further investigation with the onboard SIMBIO-SYS instrument on the BepiColombo mission will help to better understand the current state of these craters and their volatile deposits. • Novel Sun Discretization Method: We developed a unique tool that discretizes the Sun into 100 elements, allowing for more accurate modeling of solar flux on Mercury’s polar regions. • Enhanced Thermal Modeling: The study provides a refined approach to calculating temperature distribution, incorporating both direct solar illumination and self-heating effects, particularly in complex crater geometries. • Application to Mercury’s Polar Craters: Our model was applied to the Laxness and Fuller craters, revealing significant temperature variations due to self-heating, especially within permanently shadowed regions (PSRs). • Potential Impact on Water Ice Stability: While the temperature rise due to self-heating does not affect water ice stability in the Laxness crater, a section of the Fuller crater’s radar-bright material reaches temperatures that could potentially compromise water ice stability. • Future Exploration: The findings underscore the importance of revisiting these craters with the upcoming BepiColombo mission and the SIMBIO-SYS instrument to gain a deeper understanding of their thermal state.