The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
The Horizontal Wavelength Spectrum of Gravity Wave Activity in Mars’s Lower Atmosphere: The Perspective from MGS–TES Nadir Observations
复制标题
火星低层大气重力波活动的水平波长谱：来自 MGS-TES 天底观测的视角
DOI：
10.3847/psj/ac8d62
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发表时间：
2022
影响因子：
--
通讯作者：
C. Wright
中科院分区：
文献类型：
--
作者：
N. Heavens;A. Pankine;J. Battalio;C. Wright
将高层大气重力波（GW）与其低层和中层大气（0-30公里和30-100公里高度）的起源联系起来，可以提高对火星大气演化及其当前热结构和一般环流的理解。最近的一项研究利用火星勘测轨道器（MRO）上的火星气候探测器（MCS）的观测结果，描述了10-100公里水平波长的低层大气GW的气候学特征，但高层大气中观测到的GW的水平波长高达500公里，这促使人们更仔细地关注低层大气GW的水平波长谱。先前对火星全球勘测者（MGS）上的热发射光谱仪（TES）的观测进行的研究报告了广泛定义的波活动的水平波长光谱的大量年际变化，包括GW。本文利用ls = 120°-150°、火星第24年和火星第25年对MRO-MCS光谱通道重采样的MGS-TES观测资料的亮度温度变化谱，得到了波活动的水平波长谱。低层大气波活动在波长<200 km处最强，与MRO-MCS观测到的波群相似，很可能是GW活动。这种短波长的波群不同于波长为1000公里的波群，后者似乎是潮汐和行星波的混合物。我们发现，以前使用MGS-TES数据确定的GW活动的年际变化主要来自MGS-TES第一季度仪器噪声特征的变化。
Connecting upper-atmospheric gravity waves (GW) to their lower- and middle-atmospheric (0–30 and 30–100 km altitude) origins can improve understanding of the evolution of Mars’s atmosphere as well as its present thermal structure and general circulation. A recent study using observations from the Mars Climate Sounder (MCS) on board the Mars Reconnaissance Orbiter (MRO) characterized the climatology of lower-atmospheric GW with 10–100 km horizontal wavelengths, but GW observed in the upper atmosphere have horizontal wavelengths of up to 500 km, motivating more careful attention to the horizontal wavelength spectrum of lower-atmospheric GW. A previous study of observations by the Thermal Emission Spectrometer (TES) on Mars Global Surveyor (MGS) reported substantial interannual variability in the horizontal wavelength spectrum of wave activity defined broadly, including GW. Here, we derive the horizontal wavelength spectrum of wave activity from the brightness temperature variance spectrum of MGS–TES observations resampled to the MRO–MCS spectral channels during L s = 120°–150°, Mars Years 24 and 25. Lower-atmospheric wave activity is strongest at wavelengths <200 km, a population which resembles that observed by MRO–MCS and is likely GW activity. This short-wavelength population is distinct from a wave population with wavelengths >1000 km, which appears to be a mixture of tides and planetary waves. We find that interannual variability in GW activity previously identified using MGS–TES data largely arises from a change in the instrumental noise characteristics of MGS–TES during the first quarter of MY 25.
影响因子：
2.6
作者：
Erdal Yiğit;A. Medvedev
通讯作者：
Erdal Yiğit;A. Medvedev
影响因子：
3.2
作者：
Alex Siddle-;I. Mueller-Wodarg;S. Stone;R. Yelle
通讯作者：
Alex Siddle-;I. Mueller-Wodarg;S. Stone;R. Yelle