Brightness Temperature Analysis of Mare Marginis Based on CE-2 CELMS Data

Mare Marginis (13.3 N-degrees, 86.1 E-degrees) is situated on the lunar nearside with rich geological diversity. This letter analyzes the brightness temperature ( T-B ) features of Mare Marginis through the normalized brightness temperature ( nT(B) ) performances and brightness temperature difference ( dT(B) ) using data from the Chang'E-2 Lunar Microwave Sounder (CELMS), in combination with slope, rock abundance (RA), and (FeO + TiO2) abundance (FTA). The results are as follows. First, the ( nT(B) ) of Mare Marginis is relatively high at both daytime and nighttime. The daytime ( nT(B) ) shows consistency with FTA distribution. Second, the ( dT(B) ) of Mare Marginis is basically consistent with the FTA distribution, the consistency decreases as the frequency increases. Third, the correlation analysis shows that slope and FTA are the main factors influencing ( nT(B) ) . In addition, the high substrate temperature is identified as the primary factor responsible for nighttime ( nT(B) ) anomalies of Mare Marginis, whereas the high RA accounts for the emergence of the cold spot phenomenon at Goddard A crater.