Thermal anomaly spots (both hot and cold) have been found in the global 37-GHz brightness temperature (TB) map of the moon based on the Chang'E (CE) microwave radiometer measurements. To explain their origin, a rock model is proposed to simulate the TB variation against latitude along the profile of a fresh crater in a single track way, which is selected to highlight the topographic effect and avoid any modification to the data. A mixed upper layer made up of rock and soil (regolith and dust) was employed into our previous multilayer model. The thermal properties (thermal conductivity and heat capacity) of the mixture layer are presumed to be linear with the fraction of rocks. Given that high-frequency (37 GHz) measurements are chosen, only the meter size and larger rocks of the upper mixed layer are considered to avoid scattering effects. Several fresh craters poor/rich in ilmenite are selected as testing sites. Despite uncertainties in parameters such as rock abundance (RA), and iron and titanium abundances, three conclusions can be reached from these cases: 1) RA has a significant effect on both the TB value and TB variation trend against latitude; its contribution over some craters may be as high as 15 K; 2) the simulations based on our rock model fit the CE observations better than those when rocks are not included; and 3) the rock and ilmenite contributions could be the main cause for the cold and hot spots found in the CE microwave map.

Mare Moscoviense (148°E, 27°N) is one of the few large maria on the lunar farside, with the thinnest crust and a positive gravity anomaly. In this paper, the Chang’E-2 Microwave Sounder (CELMS) data was employed to study the microwave thermal emission features of mare basalts in Moscoviense Basin. The time angle and linear interpolation method are used to generate the brightness temperature (T_B) maps at noon and night, as well as the T_B difference (dT_B) map. The obtained important results are as follows. (1) A new geologic map is generated with the T_B and dT_B maps using the maximum likelihood method, which gives a new expression about the basaltic units in Mare Moscoviense compared to the optical results; (2) the substrate temperature of Moscoviense Basin is likely warmer than what we know; (3) unit Ihtm (a Late (?) Imbrian, mid- to high-Ti, high-Fe basalt) is re-understood as two independent volcanic features with their own fissures; (4) the dT_B maps firstly indicate that the depth lunar regolith is homogeneous in the highlands surrounding Mare Moscoviense, at least in the microwave domain, and secondly that there exists a special material bringing about the low dT_B anomaly in the shallow layer of the east highlands. The results will be of great significance to better understand the basaltic volcanism of the Moon.

Chang'E lunar microwave sounder (CELMS) data provide a potential way to understand the thermophysical features of the shallow lunar crust. In this study, four typical Copernican craters, including Copernicus, Aristarchus, Tycho, and Jackson, have been selected and their brightness temperature $(T_{B})$ performances are evaluated with the CE-2 CELMS data. The results are as follows. First, the hot $T_{B}$ anomaly is reunderstood according to the $T_{B}$ behaviors. The cause to the anomaly is still in doubt, and we rule out the previous explanations as rock abundance or topography. Second, the existence of the cold anomaly indicates the shallow lunar crust is likely much colder than what we knew. Third, the $T_{B}$ performances indicate that the shallow lunar crust is likely homogeneous, and the materials here have very low (FeO+TiO $_2$ ) abundance and thermal inertia. Also, the difference of the $T_{B}$ performances from the crater floors to far distance will provide a new constraint for the cratering formation study.

Apollo basin is located within the large South Pole–Aitken (SPA) basin. The study on Apollo basin will provide interesting information about the basic geologic issues about the lunar farside. In this paper, the normalized brightness $(T_{B})$ temperature $(nT_{B})$ maps and the $T_{B}$ difference $(dT_{B})$ maps are generated with the Chang'E-2 microwave sounder data to study the microwave thermal emission features of Apollo basin. The results are as follows. First, the mare volcanism in Apollo basin is re-understood according to the $nT_{B}$ performances at noon, and they should be originated from the southern part of the Apollo basin and strongly altered by the later impact ejecta. Second, the $nT_{B}$ maps indicate that there exists a special material from Dryden crater to Chaffee crater, whose thickness is more than 31 cm but less than 76.9 cm. Third, the similar $dT_{B}$ performances at 3.0 GHz indicate the homogeneous regolith thermophysical parameters of Apollo basin in the lateral direction. Fourth, the $dT_{B}$ maps and the discovered cold $T_{B}$ anomaly indicate the homogeneity of the SPA basin at least in the microwave thermophysical parameters. Our study also shows that the scientific study about the lunar surface is not sufficient only by visible data.