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首页> 外文期刊>Journal of geophysical research. Planets >The structure of Mars lower atmosphere from Mars Express Radio Science (MaRS) occultation measurements
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The structure of Mars lower atmosphere from Mars Express Radio Science (MaRS) occultation measurements

机译：火星快速无线电科学（MaRS）掩星测量的火星低层大气结构

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The Mars Express Radio Science Experiment (MaRS) investigates the lower and middle atmosphere of Mars between the surface and about 40 km with a very high vertical resolution. More than 600 profiles of temperature, pressure, and neutral number density were retrieved between 2004 and 2011 covering four Martian years (MYs 27-30). Radio occultation experiments provide the unique possibility to retrieve geopotential height information to supplement temperature values. The temperature field in the northern winter hemisphere displays strong temperature inversions indicating a pronounced polar warming in the northern polar night (MY 27). The temperature and geopotential fields imply the presence of a strong zonal jet, with peak wind speeds of more than 170 m/s at an altitude of about 30 km (~15 Pa) and a latitude of 60-65°N. The longitudinal temperature and geopotential fields in the southern winter of Martian year 30 at latitudes between 49° and 69°S are dominated by a stationary zonal wave s = 1 structure in the lower atmosphere. Associated meridional wind fields retrieved by assuming geostrophic balance have amplitudes up to 12 m/s at the 200 Pa level. An investigation of small-scale atmospheric waves reveals enhanced gravity wave activity in the daytime atmosphere above elevated terrain and in the winter extratropics. Radio occultation experiments also provide unique insight into the structure of the planetary boundary layer. The deepest convective boundary layers, up to 10 km, are found over elevated terrain. Key PointsMaRS investigates the large scale and small scale atmospheric structuresZonal and meridional wave structures are examinedGravity waves and the planetary boundary layer are invstigated.
机译：火星快速无线电科学实验（MaRS）以非常高的垂直分辨率研究了火星表面和约40 km之间的低层和中层大气。在2004年至2011年之间，共获得了600多个温度，压力和中性数密度分布图，涵盖了四个火星年（27-30 MYs）。无线电掩星实验提供了检索地势高度信息以补充温度值的独特可能性。冬季北半球的温度场显示强烈的温度反演，表明北极极夜（MY 27）出现明显的极地变暖。温度场和地势场表明存在强烈的纬向射流，在大约30 km（〜15 Pa）的海拔和60-65°N的纬度下，峰值风速超过170 m / s。火星30年南部冬季在49°和69°S之间的纬度的纵向温度和地势场由较低大气层中的固定纬向波s = 1结构决定。通过假定地转平衡获得的相关子午风场在200 Pa高度的振幅高达12 m / s。对小规模大气波的研究表明，在高海拔以上的白天大气和冬季温带气候中，重力波活动有所增强。无线电掩星实验还提供了对行星边界层结构的独特见解。在升高的地形上发现了最深的对流边界层，长达10 km。关键要点MaRS研究了大尺度和小尺度的大气结构研究了纬向和经向波结构，研究了重力波和行星边界层。

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