Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data
The rock strongly affects the surface and subsurface temperature due to its different thermophysical properties compared to the lunar regolith. The brightness temperature (TB) data observed by Chang’E-1 (CE-1) and Chang’E-2 (CE-2) microwave radiometers (MRM) give us a chance to retrieve the lunar su...
| Main Authors: | , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
MDPI AG
2023-10-01
|
| Series: | Remote Sensing |
| Subjects: | |
| Online Access: | https://www.mdpi.com/2072-4292/15/20/4895 |
| _version_ | 1797572426320576512 |
|---|---|
| author | Wei Yang Guoping Hu Fan Yang Wenchao Zheng |
| author_facet | Wei Yang Guoping Hu Fan Yang Wenchao Zheng |
| author_sort | Wei Yang |
| collection | DOAJ |
| description | The rock strongly affects the surface and subsurface temperature due to its different thermophysical properties compared to the lunar regolith. The brightness temperature (TB) data observed by Chang’E-1 (CE-1) and Chang’E-2 (CE-2) microwave radiometers (MRM) give us a chance to retrieve the lunar subsurface rock abundance (RA). In this paper, a thermal conductivity model with an undetermined parameter <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>β</mi></mrow></semantics></math></inline-formula> of the mixture has been employed to estimate the physical temperature profile of the mixed layer (rock and regolith). Parameter <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>β</mi></mrow></semantics></math></inline-formula> and the physical temperature profile of the mixed layer are constrained by the Diviner Channel 7 observations. Then, the subsurface RA on the 16 large (Diameter > 20 km) Copernican-age craters of the Moon is extracted from the average nighttime TB of the CE-2 37 GHz channel based on our previous rocky TB model. Two conclusions can be derived from the results: (1) the subsurface RA values are usually greater than the surface RA values retrieved from Diviner observations of the studied craters; (2) the spatial distribution of subsurface RA extracted from CE-2 MRM data is not necessarily consistent with the surface RA detected by Diviner data. For example, there are similar RA spatial distributions on both the surface and subsurface in Giordano Bruno, Necho, and Aristarchus craters. However, the distribution of subsurface RA is obviously different from that of surface RA for Copernicus, Ohm, Sharonov, and Tycho craters. |
| first_indexed | 2024-03-10T20:56:07Z |
| format | Article |
| id | doaj.art-dfe6f0f0d7194011bc62aeca13bb375c |
| institution | Directory Open Access Journal |
| issn | 2072-4292 |
| language | English |
| last_indexed | 2024-03-10T20:56:07Z |
| publishDate | 2023-10-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Remote Sensing |
| spelling | doaj.art-dfe6f0f0d7194011bc62aeca13bb375c2023-11-19T17:57:56ZengMDPI AGRemote Sensing2072-42922023-10-011520489510.3390/rs15204895Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature DataWei Yang0Guoping Hu1Fan Yang2Wenchao Zheng3State Key Laboratory of Lunar and Planetary Science, Macau University of Science and Technology, Macau 999078, ChinaSchool of Geospatial Engineering and Science, Sun Yat-Sen University, Zhuhai 519082, ChinaSchool of Information and Communication, National University of Defense Technology, Wuhan 430000, ChinaHubei Key Laboratory for High Efficiency Utilization of Solar Energy and Operation Control of Energy Storage System, Hubei University of Technology, Wuhan 430068, ChinaThe rock strongly affects the surface and subsurface temperature due to its different thermophysical properties compared to the lunar regolith. The brightness temperature (TB) data observed by Chang’E-1 (CE-1) and Chang’E-2 (CE-2) microwave radiometers (MRM) give us a chance to retrieve the lunar subsurface rock abundance (RA). In this paper, a thermal conductivity model with an undetermined parameter <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>β</mi></mrow></semantics></math></inline-formula> of the mixture has been employed to estimate the physical temperature profile of the mixed layer (rock and regolith). Parameter <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>β</mi></mrow></semantics></math></inline-formula> and the physical temperature profile of the mixed layer are constrained by the Diviner Channel 7 observations. Then, the subsurface RA on the 16 large (Diameter > 20 km) Copernican-age craters of the Moon is extracted from the average nighttime TB of the CE-2 37 GHz channel based on our previous rocky TB model. Two conclusions can be derived from the results: (1) the subsurface RA values are usually greater than the surface RA values retrieved from Diviner observations of the studied craters; (2) the spatial distribution of subsurface RA extracted from CE-2 MRM data is not necessarily consistent with the surface RA detected by Diviner data. For example, there are similar RA spatial distributions on both the surface and subsurface in Giordano Bruno, Necho, and Aristarchus craters. However, the distribution of subsurface RA is obviously different from that of surface RA for Copernicus, Ohm, Sharonov, and Tycho craters.https://www.mdpi.com/2072-4292/15/20/4895Chang’e-2 (CE-2)cratermicrowave brightness temperaturerock abundance (RA) |
| spellingShingle | Wei Yang Guoping Hu Fan Yang Wenchao Zheng Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data Remote Sensing Chang’e-2 (CE-2) crater microwave brightness temperature rock abundance (RA) |
| title | Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data |
| title_full | Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data |
| title_fullStr | Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data |
| title_full_unstemmed | Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data |
| title_short | Inversion of the Lunar Subsurface Rock Abundance Using CE-2 Microwave Brightness Temperature Data |
| title_sort | inversion of the lunar subsurface rock abundance using ce 2 microwave brightness temperature data |
| topic | Chang’e-2 (CE-2) crater microwave brightness temperature rock abundance (RA) |
| url | https://www.mdpi.com/2072-4292/15/20/4895 |
| work_keys_str_mv | AT weiyang inversionofthelunarsubsurfacerockabundanceusingce2microwavebrightnesstemperaturedata AT guopinghu inversionofthelunarsubsurfacerockabundanceusingce2microwavebrightnesstemperaturedata AT fanyang inversionofthelunarsubsurfacerockabundanceusingce2microwavebrightnesstemperaturedata AT wenchaozheng inversionofthelunarsubsurfacerockabundanceusingce2microwavebrightnesstemperaturedata |