Barth C A, Hord C W, Stewart A I, Lane A L
Science. 1972 Jan 21;175(4019):309-12. doi: 10.1126/science.175.4019.309.
The ultraviolet airglow spectrum of Mars has been measured from an orbiting spacecraft during a 30-day period in November-December 1971. The emission rates of the carbon monoxide Cameron and fourth positive bands, the atomic oxygen 1304-angstrom line and the atomic hydrogen 1216-angstrom line have been measured as a function of altitude. Significant variations in the scale height of the CO Cameron band airglow have been observed during a period of variable solar activity; however, the atomic oxygen and hydrogen airglow lines are present during all the observations. Measurements of the reflectance of the lower atmosphere of Mars show the spectral characteristics of particle scattering and a magnitude that is about 50 percent of that measured during the Mariner 6 and 7 experiments in 1969. The variation of reflectance across the planet may be represented by a model in which the dominant scatterer is dust that absorbs in the ultraviolet and has an optical depth greater than 1. The atmosphere above the polar region is clearer than over the rest of the planet.
1971年11月至12月的30天期间，从轨道运行的航天器上对火星的紫外气辉光谱进行了测量。测量了一氧化碳卡梅伦带和第四正带、原子氧1304埃线以及原子氢1216埃线的发射率随高度的变化情况。在太阳活动变化的时期内，观测到一氧化碳卡梅伦带气辉标高有显著变化；然而，在所有观测期间都存在原子氧和氢的气辉线。对火星低层大气反射率的测量显示出粒子散射的光谱特征，其量级约为1969年水手6号和7号实验期间测量值的50%。整个行星反射率的变化可用一个模型来表示，其中主要散射体是在紫外波段吸收且光学深度大于1的尘埃。极地地区上方的大气比行星其他区域的大气更清澈。
