论文标题
紫外线中的木星：木星在木星平流层中的乙炔和乙烷丰度，从0.15至0.19 $μ$ m之间的Cassini观测值
Jupiter in the ultraviolet: acetylene and ethane abundances in the stratosphere of Jupiter from Cassini observations between 0.15 and 0.19 $μ$m
论文作者
论文摘要
在0.15至0.19 $μ$ m之间的波长下，木星的远粉状谱谱由散射的太阳光谱支配，这主要由乙酰烯和乙烷的分子吸收减弱，并且在较小程度上是氨和氨和氨和磷酸的。我们描述了我们的辐射转移代码的发展，该代码能够从紫外线反射光谱中检索这些分子物种。作为概念验证，我们介绍了2000/2001 Flyby期间对木星磁盘的Cassini Ultraviolet成像光谱仪（UVIS）的分析。上层平流层中的紫外线乙炔丰度低于仅基于复合红外光谱仪（CIR）观察到的红外层层的红外热发射预测的乙炔丰度，需要对1 MBAR上方的垂直轮廓进行调整。我们产生了与CIR和UVIS兼容的垂直乙炔丰富度剖面，压力下的丰度降低了$ 1 MBAR：0.1 MBAR丰度为1.21 \ pm 0.07 $ 0.07 $ ppm的acetylene $ ppm and acetylene，$ 20.8 \ pm 5.1 \ pm 5.1 $ ppp for Ethane。最后，我们对果汁紫外线仪器进行了灵敏度研究，该仪器的波长覆盖范围扩大到0.21 $μ$ m，除了乙酰烯和乙烷之外，还可以检索氨和磷酸丰度。
At wavelengths between 0.15 and 0.19 $μ$m, the far-ultraviolet spectrum of Jupiter is dominated by the scattered solar spectrum, attenuated by molecular absorptions primarily by acetylene and ethane, and to a lesser extent ammonia and phosphine. We describe the development of our radiative transfer code that enables the retrieval of abundances of these molecular species from ultraviolet reflectance spectra. As a proof-of-concept we present an analysis of Cassini Ultraviolet Imaging Spectrograph (UVIS) observations of the disk of Jupiter during the 2000/2001 flyby. The ultraviolet-retrieved acetylene abundances in the upper stratosphere are lower than those predicted by models based solely on infrared thermal emission from the mid-stratosphere observed by the Composite Infrared Spectrometer (CIRS), requiring an adjustment to the vertical profiles above 1 mbar. We produce a vertical acetylene abundance profile that is compatible with both CIRS and UVIS, with reduced abundances at pressures $<$1 mbar: the 0.1 mbar abundances are $1.21 \pm 0.07$ ppm for acetylene and $20.8 \pm 5.1$ ppm for ethane. Finally, we perform a sensitivity study for the JUICE UVS instrument, which has extended wavelength coverage out to 0.21 $μ$m, enabling the retrieval of ammonia and phosphine abundances, in addition to acetylene and ethane.
