This work offers the first in‐depth study of the global characteristics of wave perturbations in temperature profiles at 20–140 km altitudes derived from the Imaging Ultraviolet Spectrograph (IUVS) onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. The peak amplitudes of waves seen in temperature profiles exceed 20% of the mean background, especially on the nightside, which is larger than those in Earth's mesosphere and thermosphere. The wave perturbations generate an instability layer around 70–100 km on the nightside, which potentially causes wave‐breaking and turbulences. Our results highlighted a seasonal variation in the latitudinal distribution of nightside perturbations. Amplitudes of wave perturbations were found to be large in the northern low‐latitude region and the southern polar region during the first half of the year (L_s = 0–180°). An increase of waves in the spectral density was found in southern low‐latitude regions in the latter half of the year (L_s = 180–360°). Vertical wavenumber spectral density in the Martian middle atmosphere shows a power‐law dependence with a logarithmic spectral slope of −3, similar to the features seen in the Earth's atmosphere. The derived spectral power density suggests the longer waves growing with height while the effective dissipation of shorter waves occurs. The strong CO₂ 15‐micron band cooling can effectively dissipate shorter waves. In contrast, the spectral power density at longer waves suggests an amplitude growth with height of unsaturated waves up to the lower thermosphere.

中文翻译：

---

MAVEN / IUVS在火星中层大气中波扰动的垂直传播

这项工作提供了对火星大气和挥发份（MAVEN）飞船上的成像紫外光谱仪（IUVS）得出的20-140 km高度的温度剖面中波扰动全球特征的首次深入研究。在温度曲线中看到的波峰幅度超过了平均背景的20％，尤其是在夜晚，这比地球的中层和热层更大。波浪的扰动会在夜间在70-100 km左右产生不稳定性层，这可能会引起波浪破裂和湍流。我们的结果突出了夜间扰动的纬度分布的季节性变化。L _s  = 0–180°）。下半年，南部低纬度地区（L _s  = 180–360°）发现频谱密度的波增加。火星中层大气的垂直波数频谱密度显示出幂律相关性，对数频谱斜率为-3，与地球大气层中的特征相似。得出的频谱功率密度表明，随着高度的增加，较长的波会增加，而较短波的有效消散会发生。强大的CO ₂ 15微米频带冷却可以有效消散较短的波。相反，在较长波处的频谱功率密度表明，随着不饱和波的高度直至较低的热圈，振幅会增大。