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• W3100970109 abstract "&lt;p&gt;We present a study of the seasonal evolution of Titan&amp;#8217;s thermal field and distributions of haze, C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;4&lt;/sub&gt;, C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;6&lt;/sub&gt;, CH&lt;sub&gt;3&lt;/sub&gt;C&lt;sub&gt;2&lt;/sub&gt;H, C&lt;sub&gt;3&lt;/sub&gt;H&lt;sub&gt;8&lt;/sub&gt;, C&lt;sub&gt;4&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, C&lt;sub&gt;6&lt;/sub&gt;H&lt;sub&gt;6&lt;/sub&gt;, HCN and HC&lt;sub&gt;3&lt;/sub&gt;N from March 2015 (Ls = 66&amp;#176;) to September 2017 (Ls = 93&amp;#176;), i.e. from the last third of northern spring to early summer. We analyzed thermal emission of Titan&amp;#8217;s atmosphere acquired by the Cassini Composite Infrared Spectrometer (CIRS) with limb and nadir geometry to retrieve the stratospheric and mesospheric temperature and mixing ratios pole-to-pole meridional cross sections from 5 mbar to 50 &amp;#956;bar (120-650 km).&lt;/p&gt; &lt;p&gt;The southern stratopause varied in a complex way and showed a global temperature increase from 2015 to 2017 at high-southern latitudes. Stratospheric southern polar temperatures, which were observed to be as small as 120 K in early 2015 due to the polar night, showed a 30-K increase (at 0.5 mbar) from March 2015 to May 2017 due to adiabatic heating in the subsiding branch of the global overturning circulation. All photochemical compounds were enriched at the South Pole by this subsidence. Polar cross sections of these enhanced species, which are good tracers of the global dynamics, highlighted changes in the structure of the southern polar vortex. These high enhancements combined with the unusually low temperatures (&lt;120 K) of the deep stratosphere resulted in condensation at the South Pole between 0.1 and 0.03 mbar (240-280 km) of HCN, HC&lt;sub&gt;3&lt;/sub&gt;N, C&lt;sub&gt;6&lt;/sub&gt;H&lt;sub&gt;6&lt;/sub&gt; and possibly C&lt;sub&gt;4&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt; in March 2015 (Ls = 66&amp;#176;). These molecules were observed to condense deeper further away from the South Pole.&lt;/p&gt; &lt;p&gt;At high-northern latitudes, stratospheric enrichments remaining from the winter were observed below 300 km between 2015 and May 2017 (Ls = 90&amp;#176;) for all chemical compounds and up to September 2017 (Ls = 93&amp;#176;) for C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;4&lt;/sub&gt;, CH&lt;sub&gt;3&lt;/sub&gt;C&lt;sub&gt;2&lt;/sub&gt;H, C&lt;sub&gt;3&lt;/sub&gt;H&lt;sub&gt;8&lt;/sub&gt;, C&lt;sub&gt;4&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;. In September 2017, these local enhancements were less pronounced than earlier for C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, C&lt;sub&gt;4&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, CH&lt;sub&gt;3&lt;/sub&gt;C&lt;sub&gt;2&lt;/sub&gt;H, HC&lt;sub&gt;3&lt;/sub&gt;N, HCN and no longer observed for C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;6 &lt;/sub&gt;and C&lt;sub&gt;6&lt;/sub&gt;H&lt;sub&gt;6&lt;/sub&gt;, which suggests a change of the northern polar dynamics near the summer solstice. These enhancements observed during the entire spring may be due to confinement of this enriched air by a small remaining winter circulation cell that persisted in the low stratosphere up to the northern summer solstice, according to predictions of the Institut Pierre Simon Laplace Titan Global Climate Model (IPSL Titan GCM).&lt;/p&gt; &lt;p&gt;In the mesosphere, we derived a depleted layer in C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, HCN and C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;6&lt;/sub&gt; from the North Pole to mid-southern latitudes, while C&lt;sub&gt;4&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt;, C&lt;sub&gt;3&lt;/sub&gt;H&lt;sub&gt;4&lt;/sub&gt;, C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;4&lt;/sub&gt; and HC&lt;sub&gt;3&lt;/sub&gt;N seem to have been enriched in the same region. In the deep stratosphere, all molecules except C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;4&lt;/sub&gt; were depleted due to their condensation sink located deeper than 5 mbar outside the southern polar vortex. HCN, C&lt;sub&gt;4&lt;/sub&gt;H&lt;sub&gt;2&lt;/sub&gt; and CH&lt;sub&gt;3&lt;/sub&gt;C&lt;sub&gt;2&lt;/sub&gt;H VMR cross section contours showed steep slopes near mid-latitudes or close to the equator, which can be explained by upwelling air in this region. Upwelling is also supported by the cross section of C&lt;sub&gt;2&lt;/sub&gt;H&lt;sub&gt;4&lt;/sub&gt; (the only molecule not condensing among those studied here) volume mixing ratio observed in the northern hemisphere.&lt;/p&gt; &lt;p&gt;We derived the zonal wind velocity up to mesospheric levels from the retrieved thermal field. We show that zonal winds were faster and more confined around the South Pole in 2015 (Ls = 67 - 72&amp;#176;) than later. In 2016, the polar zonal wind speed decreased while the fastest winds had migrated toward low-southern latitudes.&lt;br /&gt;&lt;br /&gt;&lt;/p&gt;" @default.
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• W3100970109 date "2020-10-08" @default.
• W3100970109 modified "2023-10-06" @default.
• W3100970109 title "Temperature, chemical species and wind distributions in the middle atmosphere of Titan from late northern spring to early summer" @default.
• W3100970109 doi "https://doi.org/10.5194/epsc2020-872" @default.
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