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A reanalysis of the Apollo light scattering observations, and implications for lunar exospheric dust

机译：对阿波罗光散射观测结果的重新分析及其对月球大气层尘埃的影响

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摘要

Conspicuous excess brightness, exceeding that expected from coronal and zodiacal light (CZL), was observed above the lunar horizon in the Apollo 15 coronal photographic sequence acquired immediately after orbital sunset (surface sunrise). This excess brightness systematically faded as the Command Module moved farther into shadow, eventually becoming indistinguishable from the CZL background. These observations have previously been attributed to scattering by ultrafine dust grains (radius ～0.1 microns) in the lunar exosphere, and used to obtain coarse estimates of dust concentration at several altitudes and an order-of-magnitude estimate of ～10~(-9)g cm~(-2) for the column mass of dust near the terminator, collectively referred to as model "0". We have reanalyzed the Apollo 15 orbital sunset sequence by incorporating the known sightline geometries in a Mie-scattering simulation code, and then inverting the measured intensities to retrieve exospheric dust concentration as a function of altitude and distance from the terminator. Results are presented in terms of monodisperse (single grain size) dust distributions. For a grain radius of 0.10 microns, our retrieved dust concentration near the terminator (～ 0.010 cm~(-3) is in agreement with model "0" at z=10km, as is the dust column mass (～3-6×10~(10)g cm~(-2), but the present results indicate generally larger dust scale heights, and much lower concentrations near 1 km ( < 0.08 cm~(-3) vs. a few times 0.1 cm~(-3) for model "0"). The concentration of dust at high altitudes (z>50km) is virtually unconstrained by the measurements. The dust exosphere extends into shadow a distance somewhere between 100 and 200 km from the terminator, depending on the uncertain contribution of CZL to the total brightness. These refined estimates of the distribution and concentration of exospheric dust above the lunar sunrise terminator should place new and more rigorous constraints on exospheric dust transport models, as well as provide valuable support for upcoming missions such as the Lunar Atmosphere and Dust Environment Explorer (LADEE).
机译：在轨道日落（地面日出）后立即获得的阿波罗15号日冕照相序列中，在月球地平线上方观察到了明显的超高亮度，超过了日冕和黄道光（CZL）所预期的亮度。随着命令模块进一步移入阴影，这种多余的亮度会系统地消失，最终与CZL背景变得无法区分。这些观测结果以前被归因于月球外层超细尘埃颗粒（半径约0.1微米）的散射，并用于获得多个海拔高度的尘埃浓度的粗略估计以及〜10〜（-9的数量级估计）。 ）g cm〜（-2）表示端接器附近的柱尘量，统称为模型“ 0”。通过将已知的视线几何形状合并到Mie散射模拟代码中，然后反转测得的强度以获取与海拔高度和距终结者的距离有关的大气外尘埃浓度，我们重新分析了Apollo 15轨道日落序列。结果以单分散（单粒径）粉尘分布表示。对于半径为0.10微米的颗粒，我们在终结器（〜0.010 cm〜（-3）附近获得的粉尘浓度在z = 10km时与模型“ 0”一致，粉尘柱质量（〜3-6×10则与上述一致） 〜（10）g cm〜（-2），但目前的结果表明尘埃高度通常更大，在1 km附近的浓度要低得多（<0.08 cm〜（-3）几倍于0.1 cm〜（-3 ）（对于模型“ 0”）。高空（z> 50km）上的尘埃浓度实际上不受测量值的限制，尘埃大气圈延伸到阴影中，距终结者100至200 km，具体取决于不确定的贡献这些对月球日出终结者上方大气层尘埃的分布和浓度的精确估算，应该对大气层尘埃传输模型施加新的更严格的限制，并为诸如月球大气等即将开展的任务提供有价值的支持和Dust Environment Explorer（LADEE）。

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  • 来源
    《Planetary and space science》 |2011年第14期|p.1695-1707|共13页
  • 作者

    David A. Glenar; Timothy J. Stubbs; James E. McCoy; Richard R. Vondrak;

  • 作者单位

    Department, of Astronomy, New Mexico State University, Las Cruces, NM, USA,NASA Lunar Science Institute, NASA Ames Research Center, Moffett Field, CA. USA;

    NASA Lunar Science Institute, NASA Ames Research Center, Moffett Field, CA. USA,Goddard Earth Sciences and Technology Center, University of Maryland, Baltimore County, Baltimore, MD, USA,NASA Goddard Space Flight Center, Greenbelt, MD. USA;

    NASA Johnson Space Center, Houston, TX, USA;

    NASA Lunar Science Institute, NASA Ames Research Center, Moffett Field, CA. USA,NASA Goddard Space Flight Center, Greenbelt, MD. USA;

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  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

    moon; horizon glow; optical scattering; lunar dust; lunar exosphere;

    机译：月亮;水平发光;光学散射;月尘;月球外层;

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