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首页> 外文期刊>Journal of Thermophysics and Heat Transfer >Thermal Optical Properties of Lunar Dust Simulants
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Thermal Optical Properties of Lunar Dust Simulants

机译：月尘模拟物的热光学性质

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摘要

The total reflectance spectra of lunar simulant dusts (<20 μm particles) were measured to determine their integrated solar absorptance α and their thermal emittance ε for the purpose of analyzing the effect of dust on the performance of thermal control surfaces. All of the simulants except Minnesota Lunar Simulant 1 had a wavelength-dependant reflectivity ρ(λ) near 0.10 over the wavelength range of 8-25 μm, and so are highly emitting at room temperature and lower. The anomalous behavior of Minnesota Lunar Simulant 1 was attributed to its very low glass content The 300 K emittance ε of all the lunar simulants, except Minnesota Lunar Simulant 1, ranged from 0.78 to 0.92. In all cases, the e was lower for the <20 μm particles than for larger particles reported earlier. There was considerably more variation in the lunar simulant reflectance in the solar spectral range (250-2500 nm) than in the thermal infrared. As expected, the lunar highlands simulants were more reflective in this wavelength range than the lunar mare simulants. The ε (λ) maxima at the Christiansen frequency were consistent with simulants being largely plagioclase and confirmed that, with the exception of Minnesota Lunar Simulant 1P, addition of agglutinates did not change the mineralogical character of the simulants. The α of the simulants ranged from 0.39 to 0.75. This is lower than values reported earlier for larger particles of the same simulants (0.41-0.82) and for representative mare and highlands lunar soils (0.74-0.91). Because the α of some mare simulants more closely matched that of highlands lunar soils, it is recommended that α and ε values be the criteria for choosing a simulant for assessing the effects of dust on thermal control surfaces, rather than whether a simulant has been formulated as a highlands or a mare simulant.
机译：测量月球模拟尘埃（<20μm颗粒）的全反射光谱，以确定它们的积分太阳吸收率α和它们的热辐射率ε，目的是分析尘埃对热控表面性能的影响。除明尼苏达州月球模拟物1以外的所有模拟物在8-25μm的波长范围内具有与波长相关的反射率ρ（λ）接近0.10，因此在室温及更低温度下会发射高光。明尼苏达州月球模拟物1的异常行为归因于其极低的玻璃含量。除明尼苏达州月球模拟物1以外，所有月球模拟物的300 K发射率ε介于0.78至0.92之间。在所有情况下，<20μm颗粒的e均比之前报道的较大颗粒的e低。在太阳光谱范围（250-2500 nm）中，模拟月球反射率的变化远大于热红外变化。不出所料，在这个波长范围内，月球高地模拟物比月球母模拟物更具反射性。克里斯琴森频率的ε（λ）最大值与模拟物主要是斜长石相符，并证实，除了明尼苏达州月球模拟物1P以外，添加凝集剂不会改变模拟物的矿物学特征。模拟物的α范围为0.39至0.75。这比先前报道的相同模拟物的较大颗粒（0.41-0.82）和代表性的母马和高地月球土壤（0.74-0.91）的值低。由于某些母马模拟物的α与高地月球土壤的α更紧密匹配，因此建议使用α和ε值作为选择模拟物以评估粉尘对热控制表面的影响的标准，而不是是否已制定模拟物作为高地或母马模拟物。

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  • 来源
    《Journal of Thermophysics and Heat Transfer》 |2012年第4期|573-580|共8页
  • 作者

    James R. Gaier; Shaneise Ellis; Nicole Hanks;

  • 作者单位

    NASA John H. Glenn Research Center at Lewis Field, Cleveland, Ohio 44135;

    NASA John H. Glenn Research Center at Lewis Field, Cleveland, Ohio 44135;

    NASA John H. Glenn Research Center at Lewis Field, Cleveland, Ohio 44135;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);
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