Measurements of Titan’s Stratospheric Winds during the 2009 Equinox with the eSMA

Measurements of Titan’s Stratospheric Winds during the 2009 Equinox with the eSMA
Siobhan Light, Mark Gurwell, Alexander Thelen, Nicholas Lombardo, Conor Nixon
arXiv:2404.08832v1 Announce Type: new
Abstract: Saturn’s moon Titan possesses stratospheric zonal winds that places it among a sparse class of planetary bodies known to have superrotation in their atmospheres. Few measurements have been made of these speeds in the upper stratosphere, leaving their seasonal variations still not well understood. We examined observations made with the extended Submillimeter Array (eSMA) in 2009 March (Ltextsubscript{s}=355textdegree{}) and 2010 February (Ltextsubscript{s}=5textdegree{}), shortly before and after Titan’s northern spring equinox. Cassini observations and atmospheric models find equinoctial periods to be especially dynamic. Zonal wind calculations, derived from the Doppler frequency shift of CHtextsubscript{3}CN near 349.4 GHz, yielded speeds of 128 $pm$ 27 m stextsuperscript{-1} in 2009 and 209 $pm$ 48 m stextsuperscript{-1} in 2010. We estimated the measured emission to originate from vertical altitudes of $336^{+112}_{-88}$ kilometers, equivalent to pressures of $3.8^{+19.2}_{-3.4}$ Pa, commensurate with Titan’s upper stratosphere/lower mesosphere. This suggests a possible increase in zonal speeds during this period. The results are then compared to those from previous Cassini-inferred and direct-interferometric observations of winds, as well as general circulation model simulations, to form a more complete picture of the seasonal cycle of stratospheric zonal winds.arXiv:2404.08832v1 Announce Type: new
Abstract: Saturn’s moon Titan possesses stratospheric zonal winds that places it among a sparse class of planetary bodies known to have superrotation in their atmospheres. Few measurements have been made of these speeds in the upper stratosphere, leaving their seasonal variations still not well understood. We examined observations made with the extended Submillimeter Array (eSMA) in 2009 March (Ltextsubscript{s}=355textdegree{}) and 2010 February (Ltextsubscript{s}=5textdegree{}), shortly before and after Titan’s northern spring equinox. Cassini observations and atmospheric models find equinoctial periods to be especially dynamic. Zonal wind calculations, derived from the Doppler frequency shift of CHtextsubscript{3}CN near 349.4 GHz, yielded speeds of 128 $pm$ 27 m stextsuperscript{-1} in 2009 and 209 $pm$ 48 m stextsuperscript{-1} in 2010. We estimated the measured emission to originate from vertical altitudes of $336^{+112}_{-88}$ kilometers, equivalent to pressures of $3.8^{+19.2}_{-3.4}$ Pa, commensurate with Titan’s upper stratosphere/lower mesosphere. This suggests a possible increase in zonal speeds during this period. The results are then compared to those from previous Cassini-inferred and direct-interferometric observations of winds, as well as general circulation model simulations, to form a more complete picture of the seasonal cycle of stratospheric zonal winds.