Tidal variations in the Martian lower atmosphere inferred from Mars Express Planetary Fourier Spectrometer temperature data
Tidal variations in the Martian lower atmosphere inferred from Mars Express Planetary Fourier Spectrometer temperature data
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根据火星快车行星傅里叶光谱仪温度数据推断出火星低层大气的潮汐变化
DOI：
10.1029/2011gl050348
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发表时间：
2011
影响因子：
5.2
通讯作者：
D.Grassi
中科院分区：
文献类型：
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作者：
Takao M.Sato;H.Fujiwara;Y.O.Takahashi;Y.Kasaba;V.Formisano;M.Giuranna;D.Grassi
我们使用火星快车（MEX）行星傅立叶光谱仪（PFS）温度数据报告了火星低层大气（<45 km）潮汐变化的特征，大约三个火星年（MY 26和MY 29结束之间）。PFS数据，广泛覆盖当地时间，使我们能够调查在不同高度的大气温度的日变化。我们专注于在一个固定的当地时间框架内的大气温度和纵向温度变化的日变化。结果表明，沙尘暴期间（Ls= 30°-60°）0.52 mbar（0.25 km）的纬向变化和日变化与以往数值模拟结果一致。在热带地区的日变化作为高度的函数的特点也解释了迁移的日潮传播的结果。研究了MY 28年北方夏至（Ls= 76°-83°）附近赤道地区（10°S-5°S）昼侧（14.36-14.94 LT）温度的经向变率。纵向温度结构在2.85毫巴（10公里）处有两个局部最大值，但在0.52毫巴处相对均匀。我们发现，在目前的情况下，波-3结构在0.11毫巴（约40公里）处是明显的。这种结构将强烈依赖于大气波的活动，例如，昼夜Kelvin波2（DK2）。
We report on the characteristics of tidal variations in the Martian lower atmosphere (<45 km) using the Mars Express (MEX) Planetary Fourier Spectrometer (PFS) temperature data for about three Martian years (between the ends of MY26 and MY29). The PFS data, which widely cover local time, enable us to investigate diurnal variations in the atmospheric temperature at various altitudes. We focus on diurnal variations in the atmospheric temperature and on longitudinal temperature variability in a fixed local time frame. We find that the latitudinal and diurnal variations at 0.52 mbar (∼25 km) during the dust‐clear period (Ls= 30°–60°) are consistent with general characteristics presented by previous numerical simulations. The characteristics of the diurnal variations as a function of altitude in the tropics are also explained as results from the propagation of the migrating diurnal tide. The longitudinal temperature variability in the dayside (14.36–14.94 LT) equatorial regions (10°S–5°S) near the northern summer solstice (Ls= 76°–83°) in MY28 are investigated. The longitudinal temperature structure has two local maxima at 2.85 mbar (∼10 km) but is relatively uniform at 0.52 mbar. We find that the wave‐3 structure is apparent at 0.11 mbar (∼40 km) in the present case. This structure would be strongly dependent on activities of the atmospheric waves, e.g., the diurnal Kelvin wave 2 (DK2).