Abstract
Lunar surface temperature is one of the fundamental thermophysical parameters of the lunar regolith, which is of great significance to the interpretation of remote-sensing thermal data. In this study, a daytime surface temperature model is established focusing on the lunar superficial layer with high spatial-temporal resolution. The physical parameters at the time of interest are adopted, including effective solar irradiance, lunar libration, large-scale topographic shading, and surrounding diffuse reflection. Thereafter, the 1/64° temperature distributions at five local times are quantitatively generated and analyzed in Sinus Iridum. Also, combined with Chang’E-2 microwave radiometer (CELMS) data and Diviner thermal infrared (TIR) data, the spectral emissivity distributions are estimated as a potential geological application of the simulated surface temperature. The results are as follows: (1) daytime surface temperature in Sinus Iridum is significantly affected by the local topography and observation time, and the influence of diffuse reflection energy is obvious; (2) the emissivity distributions provide a new way to understand the thermophysical properties difference of lunar regolith at different depths; (3) the influence of lunar orbiting revolution and precession on surface temperature should be analyzed carefully, which shows the importance of using the parameters at the time of interest.
Highlights
Lunar surface temperature is one of the important and fundamental parameters to interpret the thermal characteristics of the regolith from remote-sensing thermal data, which will give clues for solving thermal models and understanding the evolution of the Moon [1,2,3,4,5]
Based on the Stefan–Boltzmann rule, above relationship can be described by the following equation [7,32]: (1 − α)(Is + Ie + Ire f ) + εF + Qout = εσT4 + Ks (∂T/∂x) where α is the lunar surface albedo, Is is the direct effective solar irradiance, Ie is the Earth irradiance, Iref is the multiple scattering of solar radiation, ε is the infrared surface emissivity, F is the thermal energy of surrounding infrared emission, Qout is the heat flow energy from the interior of the Moon to the surface. σ is the Stefan–Boltzmann constant, T is the superficial layer temperature, Ks (∂T/∂x) is energy from the surface to the subsurface, Ks is the surface conductivity
A daytime surface temperature model is established focusing on the lunar superficial layer with high spatial-temporal resolution
Summary
Lunar surface temperature is one of the important and fundamental parameters to interpret the thermal characteristics of the regolith from remote-sensing thermal data, which will give clues for solving thermal models and understanding the evolution of the Moon [1,2,3,4,5]. Because the measurements from the orbital explorer are acquired in a very short time, the acquisition of lunar superficial layer temperature at the time of interest is indispensable in the in-situ lunar exploration but of great significance for the remote-sensing thermal data. Data, the solar albedo and large-scale topographic effect can be further introduced to simulate a more accurate surface temperature distribution [2,3,4,5,7] These surface temperature models are constantly improved, these results are not combined with the physical parameters at the time of interest, and the effects of complex surrounding thermal environment and lunar libration are not mentioned.
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
