Over the extreme temperature variations experienced in a single lunar day (∆T ≈ 300 K), particular minerals common to the lunar surface show spectral changes at discrete near‐infrared wavelengths in laboratory settings (Roush & Singer, 1986, 1987, https://10.1111/10.1029/JB091iB10p10301, https://10.1111/10.1016/0019-1035(87)90026-1; Singer & Roush, 1985, https://10.1111/10.1029/JB090iB14p12434). Variations in temperature can cause variations in the size and shape of crystallographic sites, which control the position, shape, and depth of crystal field absorptions. At an observation wavelength of 1,064 nm, the Lunar Orbiter Laser Altimeter (LOLA) should be highly sensitive to temperature‐dependent changes of orthopyroxene. Here we analyze temperature‐dependent spectral changes of the lunar surface as measured from orbit by LOLA. We couple LOLA measurements of normal albedo with measurements of surface temperature from the Diviner Lunar Radiometer Experiment, analyzing the maria and highlands between ±50°. We provide the first evidence of temperature‐dependent spectral changes on the lunar surface from orbital observations, finding that the majority of the surface between ±50° demonstrates a small, yet measurable, negative change in 1,064‐nm albedo with temperature (−∆R/∆T). The measurable effect is on the order of a few percent change in reflectance per ~80 K, indicating that temperature changes do not have a large effect on measurements of albedo at the sensitivity of the LOLA instrument. Stronger −∆R/∆T values tend to be associated with regions with elevated orthopyroxene, and the maria typically have higher levels of orthopyroxene and stronger −∆R/∆T values than the highlands. Our results suggest that single‐wavelength lasers may be powerful tools for understanding the distribution of particular minerals on the lunar surface.

中文翻译：

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1,064 nm月球正常反照率的温度相关变化

在单个阴历日经历的极端温度变化（∆ T ≈300 K），月球表面常见的特定矿物在实验室环境中在离散的近红外波长处显示光谱变化（Roush＆Singer，1986，1987，https：//10.1111/10.1029/JB091iB10p10301，https：//10.1111/10.1016 / 0019-1035（87）90026-1; Singer＆Roush，1985，https：//10.1111/10.1029/JB090iB14p12434）。温度的变化会导致晶体学位置大小和形状的变化，从而控制晶体场吸收的位置，形状和深度。在1,064 nm的观测波长下，月球轨道激光测高仪（LOLA）对邻苯二酚的温度依赖性变化高度敏感。在这里，我们分析了LOLA从轨道测得的月球表面温度相关光谱变化。我们将正常反照率的LOLA测量值与Diviner Lunar辐射计实验的表面温度测量值相结合，分析了±50°之间的玛丽亚和高地。我们通过轨道观测提供了月球表面温度相关光谱变化的第一个证据，发现在±50°之间的大部分表面在1,064 nm反射率下随温度（−∆）表现出微小但可测量的负变化。R / ∆ T）。可测量的效果大约是每80 K反射率有百分之几的变化，这表明在LOLA仪器的灵敏度下，温度变化对反照率的测量影响不大。较高的−∆ R / ∆ T值往往与邻苯二甲酚含量较高的地区有关，并且与高地相比，玛丽亚地区通常具有较高的邻苯二酚含量和较高的−∆ R / ∆ T值。我们的结果表明，单波长激光可能是了解月球表面特定矿物分布的有力工具。