Rohini S. Giles

Latitudinal variability in Jupiter’s tropospheric disequilibrium species: GeH4, AsH3 and PH3

Giles was supported via a Royal Society studentship, and Fletcher was supported via a Royal Society Research Fellowship at the University of Leicester. Irwin acknowledges the support of the United Kingdom Science and Technology Facilities Council. This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 090.C-0053(A).

Detection of H3+ auroral emission in Jupiter's 5-micron window

We use high-resolution ground-based observations from the VLT CRIRES instrument in December 2012 to identify sixteen previously undetected H3+ emission lines from Jupiters ionosphere. These emission lines are located in Jupiters 5-micron window (4.5-5.2 {\mu}m), an optically-thin region of the planets spectrum where the radiation mostly originates from the deep troposphere. The H3+ emission lines are so strong that they are visible even against this bright background. We measure the Doppler broadening of the H3+ emission lines in order to evaluate the kinetic temperature of the molecules, and we obtain a value of 1390

Moist Convection and the 2010-2011 Revival of Jupiter's South Equatorial Belt

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Jupiter’s North Equatorial Belt expansion and thermal wave activity ahead of Juno’s arrival

160 K. We also measure the relative intensities of lines in the {\nu}2 fundamental in order to calculate the rotational temperature, obtaining a value of 960

Assessing the long-term variability of acetylene and ethane in the stratosphere of Jupiter

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Mid-infrared mapping of Jupiter’s temperatures, aerosol opacity and chemical distributions with IRTF/TEXES

40 K. Finally, we use the detection of an emission line from the 2{\nu}2(2)-{\nu}2 overtone to measure a vibrational temperature of 925

The origin of nitrogen on Jupiter and Saturn from the 15N/14N ratio

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Seasonal evolution of Saturn's polar temperatures and composition

25 K. We use these three independent temperature estimates to discuss the thermodynamic equilibrium of Jupiters ionosphere.

Cloud structure and composition of Jupiter’s troposphere from 5-μm Cassini VIMS spectroscopy

Fletcher was supported by a Royal Society Research Fellowship at the University of Leicester, Giles was supported by a Royal Society research grant at the University of Oxford. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). A portion of this work was performed by Orton and Payne at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research used the ALICE High Performance Computing Facility at the University of Leicester. We are extremely grateful for the combined efforts of the numerous amateur observers (including those listed in the figure captions) for sharing their data, and for the JUPOS software developed by Grischa Hahn and Hans-Jorg Mettig to reproject the visible-light data. ¨ This investigation was partially based on thermal-infrared observations acquired at (i) the ESO Very Large Telescope Paranal UT3/Melipal Observatory using Directors Discretionary Time (program ID 286.C-5009) and regular service time (program ID 087.C-0024); (ii) the Subaru Telescope, which is 27 operated by the National Astronomical Observatory of Japan (program ID O11154); (iii) NASA’s Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration (program IDs 2010B010, 2011A010, 2011B027); and (iv) observations obtained at the Gemini Observatory (program IDs GN-2010B-DD-3, GS-2010B-Q-8 and GS-2011AQ-11), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog´ia e Innovacion Productiva (Argentina), and ´ Ministerio da Ci ´ encia, Tecnologia e Inovac¸ ˆ ao (Brazil). We wish ˜ to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

Independent evolution of stratospheric temperatures in Jupiter's northern and southern auroral regions from 2014 to 2016

The dark colors of Jupiters North Equatorial Belt (NEB, 7–17°N) appeared to expand northward into the neighboring zone in 2015, consistent with a 3–5 year cycle. Inversions of thermal-IR imaging from the Very Large Telescope revealed a moderate warming and reduction of aerosol opacity at the cloud tops at 17–20°N, suggesting subsidence and drying in the expanded sector. Two new thermal waves were identified during this period: (i) an upper tropospheric thermal wave (wave number 16–17, amplitude 2.5 K at 170 mbar) in the mid-NEB that was anticorrelated with haze reflectivity; and (ii) a stratospheric wave (wave number 13–14, amplitude 7.3 K at 5 mbar) at 20–30°N. Both were quasi-stationary, confined to regions of eastward zonal flow, and are morphologically similar to waves observed during previous expansion events.