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.

The Von Kármán crater is one of the candidate landing sites of Chinese CE-4 mission. An effective solar radiation model was established through the improvement of the lunar illumination model based on LOLA data. Then the solar radiation condition of Von Kármán crater in 2018 was numerically simulated and analyzed. The results are as followings. Firstly，the topography strongly impacts the solar radiation，that is，there is more solar radiation in the south crater wall，the north side of the central peak and the south wall of the small craters. What’s more，the solar radiation energy received by the most areas of bottom plain is about （0.9~1）×1010 J/m2. Also，the solar radiation is more easily affected by latitude without considering the surface slope，the range of which is between 0.87 to 1.01×1010 J/m2 from the north end to the south. Thereafter，two candidate landing areas，named regions S1 and S2，were proposed based on surface slope and illumination conditions. The Region S1 is located in the bottom of the southern plain with more flat terrain，sunrise earlier and longer illumination time；while the Region S2 is located in the northwest side of the central peak with more solar radiation energy. The annual average solar radiation energy of the two regions are 9.31×109 J/m2 and 9.65×109 J/m2，respectively. The longest illumination time is in July，which is more suitable for landing.

The illumination analysis algorithm at mid-low latitudes is improved. Taking Aristarchus plateau （AP） as an example，the high resolution and high accuracy LOLA data from the LRO satellite and DE/LE430 lunar planetary ephemeris are used to quantitatively calculate and analyze the illumination characteristics of AP based on the Moon’s libration model. The results show that the illumination rates of AP area are all over 0.35，and the illumination condition of flat area is good. The illumination rates vary greatly in different regions because of the influence of terrain. The maximum illumination rate is higher than the minimum above 30%. Considering the typical long term libration effects，the results of 18.6 years show that the change of illumination rate is small and stable，which is an important reference for the research on the evolution of the lunar surface.

Mare Orientale is the youngest and best-preserved multiring impact basin, whose microwave thermal emission (MTE) research has great significance for studying the internal thermal features and thermal structures of the lunar surface. In this paper, the microwave sounder (Chang'E Lunar Microwave Sounder, CELMS) data from Chang'E-2 satellite were used to study the MTE features of the Mare Orientale. The results indicate that the MTE features of the lunar regolith are much different between those in the superficial layer and in the substrate layer. Also, substrate temperature in the Orientale Basin is likely much higher than what we know. In addition, a new perspective is given to the Hevelius Formation, which is divided into the northeastern, northwestern, and southern parts, and has several potential linear structures. The results are of substantial geologic importance to study the thermal evolution of the Moon.

Tycho撞击坑作为月球最具代表性的哥白尼纪撞击坑,其微波热辐射特性的研究对于分析与其同期形成的大型撞击坑的热演化过程具有重要的参考价值.本文基于嫦娥二号微波辐射计(CELMS)数据为代表的月壤微波热辐射数据,结合月壤TiO2含量、表面坡度和粗糙度、岩块丰度等资料,系统分析了Tycho地区微波热辐射的特征.结果表明,Tycho撞击坑南坡(A区)的微波热辐射受月表温度影响很大,月壤表层和深部的温度差值也很大;坑底平原北部(B区)的微波热辐射受月表温度影响很小,月壤表层和深部的温度差值也很小;该东部和西部的月壤结构在垂直方向上是有变化的;在凌晨3时以后该区达到热平衡状态,是未来进一步研究月壤内部热流特性的理想区域;溅射毯地区月壤物质在表层与B区相近,且具有较强的储热能力.统计结果表明,表面粗糙度和岩块丰度对月壤微波热辐射的影响最大,坡度次之,TiO2含量的影响最小.