A thermal oscillation in Jupiter’s equatorial stratosphere, thought to have ∼4 Earth year period, was first discovered in 7.8 μm imaging observations from the 1980s and 1990s. Such imaging observations were sensitive to the 10–20 hPa pressure region in the atmosphere. More recent 7.8 μm long-slit high-spectroscopic observations from 2012 to 2017 taken using the Texas Echelon cross-dispersed Echelle Spectrograph (TEXES), mounted on the NASA Infrared Telescope Facility (IRTF), have vertically resolved this phenomenon’s structure, and show that it spans a range of pressure from 2 to 20 hPa. The TEXES instrument was mounted on the Gemini North telescope in March 2017, improving the diffraction-limited spatial resolution by a factor of ∼2.5 compared with that offered by the IRTF. This Gemini spatial scale sensitivity study was performed in support of the longer-termed Jupiter monitoring being performed at the IRTF. We find that the spatial resolution afforded by the smaller 3 m IRTF is sufficient to spatially resolve the 3D structure of Jupiter’s equatorial stratospheric oscillation by comparing the thermal retrievals of IRTF and Gemini observations. We then performed numerical simulations in a general circulation model to investigate how the structure of Jupiter’s stratosphere responds to changes in the latitudinal extent of wave forcing in the troposphere. We find our simulations produce a lower limit in meridional wave forcing of 7 (planetocentric coordinates) centered about the equator. This likely remains constant over time to produce off-equatorial thermal oscillations at 13, consistent with observations spanning nearly four decades.

在木星的赤道平流层的热振荡，认为有约为4地球年的时间，在7.8首次发现μ从20世纪80年代和90年代米成像观测。这种成像观测对大气中 10-20 hPa 的压力区域很敏感。最近的 7.8 μ使用安装在 NASA 红外望远镜设施 (IRTF) 上的 Texas Echelon 交叉色散阶梯光谱仪 (TEXES) 于 2012 年至 2017 年进行的 m 长缝高光谱观测，垂直解析了这种现象的结构，并表明它跨越了压力范围为 2 至 20 hPa。TEXES 仪器于 2017 年 3 月安装在 Gemini North 望远镜上，与 IRTF 提供的分辨率相比，衍射极限空间分辨率提高了约 2.5 倍。进行这项双子座空间尺度敏感性研究是为了支持在 IRTF 进行的长期木星监测。我们发现，通过比较 IRTF 和双子座观测的热反演，较小的 3 m IRTF 提供的空间分辨率足以在空间上解析木星赤道平流层振荡的 3D 结构。然后，我们在一般环流模型中进行了数值模拟，以研究木星平流层的结构如何响应对流层中波浪强迫的纬度范围的变化。我们发现我们的模拟产生了以赤道为中心的 7（地心坐标）子午波强迫的下限。这可能会随着时间的推移保持不变，以产生 13 度的赤道外热振荡，这与跨越近 4 个十年的观测结果一致。然后，我们在一般环流模型中进行了数值模拟，以研究木星平流层的结构如何响应对流层中波浪强迫的纬度范围的变化。我们发现我们的模拟产生了以赤道为中心的 7（地心坐标）子午波强迫的下限。这可能会随着时间的推移保持不变，以产生 13 度的赤道外热振荡，这与跨越近 4 个十年的观测结果一致。然后，我们在一般环流模型中进行了数值模拟，以研究木星平流层的结构如何响应对流层中波浪强迫的纬度范围的变化。我们发现我们的模拟产生了以赤道为中心的 7（地心坐标）子午波强迫的下限。这可能会随着时间的推移保持不变，以产生 13 度的赤道外热振荡，这与跨越近 4 个十年的观测结果一致。