Evolution of lunar polar ice stability

Siegler, M. A.; Paige, D. A.; Williams, Jeffrey F.; Bills, B. G.

doi:10.1016/j.icarus.2014.09.037

Cited by 78 publications

(50 citation statements)

References 44 publications

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“…The current, and only, lunar MIR instrument is the Diviner Lunar Radiometer Experiment (Diviner) on the Lunar Reconnaissance Orbiter. Diviner measures radiance from 0.3 to 400 μm, which can be converted to emissivity to inform us about the bulk silicate mineralogy across the surface of the Moon (Greenhagen et al, ; Paige, Foote, et al, ), as well as the thermophysical properties of the lunar regolith (e.g., Bandfield et al, , ; Elder et al, ; Paige, Siegler, et al, ; Siegler et al, , ; Vasavada et al, ). Diviner has contributed to a better understanding of lunar geology, such as highly silicic features (e.g., Glotch et al, ), crater peak compositions (e.g., Song et al, ), and lunar swirls (e.g., Glotch et al, ) and shown how well Diviner data can complement visible to near‐infrared data, such as the assessment of lunar crystalline plagioclase (e.g., Donaldson Hanna et al, ), examination of volcanics (e.g., Bennett et al, ), and quantification of olivine content (e.g., Arnold et al, ).…”

Section: Introductionmentioning

confidence: 99%

Particle Size Effects on Mid‐Infrared Spectra of Lunar Analog Minerals in a Simulated Lunar Environment

Shirley

Glotch

2019

JGR Planets

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Mid‐infrared spectroscopic analysis of the Moon and other airless bodies requires a full accounting of spectral variation due to the unique thermal environment in airless body regoliths and the substantial differences between spectra acquired under airless body conditions and those measured in an ambient environment on Earth. Because there exists a thermal gradient within the upper hundreds of microns of lunar regolith, the data acquired by the Diviner Lunar Radiometer Experiment are not isothermal with wavelength. While this complication has been previously identified, its effect on other known variables that contribute to spectral variation, such as particle size and porosity, have yet to be well characterized in the laboratory. Here we examine the effect of particle size on mid‐infrared spectra of silicates common to the Moon measured within a simulated lunar environment chamber. Under simulated lunar conditions, decreasing particle size is shown to enhance the spectral contrast of the Reststrahlen bands and transparency features, as well as shift the location of the Christiansen feature to longer wavelengths. This study shows that these variations are detectable at Diviner spectral resolution and emphasizes the need for simulated environment laboratory data sets, as well as hyperspectral mid‐infrared instruments on future missions to airless bodies.

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Section: Introductionmentioning

confidence: 99%

Particle Size Effects on Mid‐Infrared Spectra of Lunar Analog Minerals in a Simulated Lunar Environment

Shirley

Glotch

2019

JGR Planets

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“…Diviner measurements offer a more accurate source of surface temperatures on the Moon throughout the diurnal cycle compared with theoretical temperature models. Although extensive analysis of surface temperature and regolith thermal properties has been performed based on Diviner data (e.g., Bandfield et al, ; Hayne et al, ; Paige et al, ; Vasavada et al, ; Williams et al, ), there are few systematic investigations of subsurface temperature as constrained by Diviner measurements (Hayne et al, ; Siegler et al, ). In this study, we present a new method to improve the accuracy of MRM T B modeling, based on Diviner data.…”

Section: Introductionmentioning

confidence: 99%

A New Method for Simulation of Lunar Microwave Brightness Temperatures and Evaluation of Chang'E‐2 MRM Data Using Thermal Constraints From Diviner

Wei

Hong

et al. 2019

JGR Planets

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We used the bolometric brightness temperatures (TBol) derived from the Lunar Reconnaissance Orbiters Diviner Lunar Radiometer (Diviner) as an upper boundary condition in our thermal model. We then calculated temperature profiles at any local time based on our improved thermal model at low to middle latitudes (70° N/S). Based on the temperature profiles, we modeled the midnight brightness temperature at 19.35 (TB19) and 37 GHz (TB37). Comparing to the Chang'E‐1 and Chang'E‐2 (CE‐1/2) observations, we found that CE‐1 showed a better data quality than that of CE‐2, especially for the TB37 data. Assuming that the issue with the CE‐2 data is caused by heat contamination of the cold‐reference antennas, we performed an empirical normalization of the CE‐2 microwave radiometer data near midnight following the approach of Hu et al. (2017). The results show that TB difference (modeled values minus modified TB) for 19.35 GHz is less than 3.40 K for ∼80% of the pixels. At 37 GHz, ∼67% of the pixels have TB difference less than 2.88 K. Additionally, we identified some areas of low microwave temperature in our modified TB maps. These low‐TB features can be characterized by two types: (1) low TB spots at fresh craters with high rock abundance and bright rays and (2) high‐Ti lunar mare surfaces with a low content of rock fragments. Investigating these low‐TB regions with the modified TB data can reveal more information about subsurface thermal regime and properties and help us better understand the evolution of regolith on the Moon.

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“…Siegler et al [] conclude that lunar obliquity history has dramatically altered the lunar polar thermal environment. In the following work, Siegler et al [] found that when the Moon was at approximately half of its current semimajor axis (3 ± 1 Gyr), lunar obliquity may have reached as high as 77°. At that time, lunar polar temperatures were much higher and cold traps could not exist.…”

Section: Introductionmentioning

confidence: 99%

Ceres's obliquity history and its implications for the permanently shadowed regions

Ermakov

Mazarico

Schröder

et al. 2017

Geophysical Research Letters

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Due to the small current obliquity of Ceres (ε≈4°), permanently shadowed regions (PSRs) exist on the dwarf planet's surface. Since the existence and persistence of the PSRs depend on the obliquity, we compute the obliquity history over the last 3 Myr and find that it undergoes large oscillations with a period of 24.5 kyr and a maximum of εmax≈19.6°. During periods of large obliquity, most of the present‐day PSRs receive direct sunlight. Some craters in Ceres's polar regions possess bright crater floor deposits (BCFDs). We find an apparent correlation between BCFDs and the most persistent PSRs. In the north, only two PSRs remain at εmax and they both contain BCFDs. In the south, one of the two only craters that remain in shadow at εmax contains a BCFD. The location of BCFDs within persistent PSRs strongly suggests that BCFDs consist of volatiles accumulated in PSR cold traps: either water molecules trapped from the exosphere or exposed ground ice.

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Evolution of lunar polar ice stability

Cited by 78 publications

References 44 publications

Particle Size Effects on Mid‐Infrared Spectra of Lunar Analog Minerals in a Simulated Lunar Environment

Particle Size Effects on Mid‐Infrared Spectra of Lunar Analog Minerals in a Simulated Lunar Environment

A New Method for Simulation of Lunar Microwave Brightness Temperatures and Evaluation of Chang'E‐2 MRM Data Using Thermal Constraints From Diviner

Ceres's obliquity history and its implications for the permanently shadowed regions

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