The vertical structure of limb hazes in the Martian atmosphere
The vertical structure of limb hazes in the Martian atmosphere
复制标题
火星大气中边缘雾的垂直结构
DOI：
10.1016/0019-1035(86)90050-3
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发表时间：
1986
期刊：
影响因子：
3.2
通讯作者：
R. Kahn
中科院分区：
文献类型：
--
作者：
F. Jaquin;P. Gierasch;R. Kahn
来自 100 多张维京轨道飞行器图像的行星边缘上方的散射光轮廓被用来限制悬浮在火星大气中的气溶胶的时间和空间行为。这些数据涵盖了广泛的季节、地点和观察几何形状，提供了有关气溶胶光学特性和垂直分布的信息。数据垂直分辨率约为1.5公里，绝对高程精度为1至4公里。 Viking Orbiter 相机校准算法可提供高达 7% 的绝对反射率精度，从而实现有意义的辐射分析。典型的大气柱在海拔 30 至 90 公里之间包含一个或多个离散的、光学薄的、冰状的雾霾层，具体取决于季节，其成分被推断为水冰。在分离的雾气下面有一个连续的雾气延伸到表面。在 50 公里以上的地方很少观察到连续的雾霾，并且颜色比上面的分离雾霾要红得多，这意味着其成分具有很强的灰尘成分。气溶胶分布表现出强烈的季节性控制，推断是由火星轨道周围可变的太阳通量驱动的。
Profiles of scattered light above the planetary limb from over 100 Viking Orbiter images are used to constrain the temporal and spatial behavior of earosols suspended in the Martian atmosphere. The data cover a wide range of seasons, locations, and viewing geometry, providing information about the aerosol optical properties and vertical distribution. The vertical resolution of the data is about 1.5 km, with an absolute elevation accuracy of 1 to 4 km. Viking Orbiter camera colibration algorithms provided reflectance accuracies to 7% absolute allowing meaningful radiometric analysis. The typical atmospheric column contains one or more discrete, optically thin, ice-like haze layers between 30 and 90 km elevation, depending on season, whose composition is inferred to be water ice. Below the detached hazes there is a continuous haze extending to the surface. The continuous haze is rarely observed above 50 km and is much redder in color than the detached hazes above, implying a composition that has a strong dust component. The aerosol distribution exhibits a strong seasonal control inferred to be driven by the variable solar flux around the orbit of Mars.