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Kim, S.J.,Geballe, T.R.,Seo, H.J.,Kim, J.H. Academic Press 2009 Icarus Vol.202 No.1
Jupiter exhibits bright H<SUP>+</SUP><SUB>3</SUB> auroral arcs at 3-4 microns that cool the hot (>1000 K) ionosphere above the ~10<SUP>-7</SUP> bar level through the infrared bands of this trace constituent. Below the 10<SUP>-7</SUP> bar level significant cooling proceeds through infrared active bands of CH<SUB>4</SUB>, C<SUB>2</SUB>H<SUB>2</SUB>, and C<SUB>2</SUB>H<SUB>6</SUB>. We report the discovery of 3-micron line emission from these hydrocarbon species in spectra of the jovian south polar region obtained on April 18 and 20, 2006 (UT) with CGS4 on the United Kingdom Infrared Telescope. Estimated cooling rates through these molecules are 7.5x10<SUP>-3</SUP>, 1.4x10<SUP>-3</SUP>, and 0.72x10<SUP>-3</SUP> Wm<SUP>-2</SUP>, respectively, for a total nearly half that of H<SUP>+</SUP><SUB>3</SUB>. We derive a temperature of 450@?+/-@?50 K in the 10<SUP>-7</SUP>-10<SUP>-5</SUP> bar region from the C<SUB>2</SUB>H<SUB>2</SUB> lines.
Kim, S.J.,Geballe, T.R.,Kim, J.H.,Jung, A.,Seo, H.J.,Minh, Y.C. Academic Press 2010 Icarus Vol.208 No.2
We present latitudinally-resolved high-resolution (R=37,000) pole-to-pole spectra of Jupiter in various narrow longitudinal ranges, in spectral intervals covering roughly half of the spectral range 2.86-3.53μm. We have analyzed the data with the aid of synthetic spectra generated from a model jovian atmosphere that included lines of CH<SUB>4</SUB>, CH<SUB>3</SUB>D, NH<SUB>3</SUB>, C<SUB>2</SUB>H<SUB>2</SUB>, C<SUB>2</SUB>H<SUB>6</SUB>, PH<SUB>3</SUB>, and HCN, as well as clouds and haze. Numerous spectral features of many of these molecular species are present and are individually identified for the first time, as are many lines of H<SUB>3</SUB><SUP>+</SUP> and a few unidentified spectral features. In both polar regions the 2.86-3.10-μm continuum is more than 10 times weaker than in spectra at lower latitudes, implying that in this wavelength range the single-scattering albedos of polar haze particles are very low. In contrast, the 3.24-3.53μm the weak polar and equatorial continua are of comparable intensity. We derive vertical distributions of NH<SUB>3</SUB>, C<SUB>2</SUB>H<SUB>2</SUB> and C<SUB>2</SUB>H<SUB>6</SUB>, and find that the mixing ratios of NH<SUB>3</SUB> and C<SUB>2</SUB>H<SUB>6</SUB> show little variation between equatorial and polar regions. However, the mixing ratios of C<SUB>2</SUB>H<SUB>2</SUB> in the northern and southern polar regions are ∼6 and ∼3 times, respectively, less than those in the equatorial regions. The derived mixing ratio curves of C<SUB>2</SUB>H<SUB>2</SUB> and C<SUB>2</SUB>H<SUB>6</SUB> extend up to the 10<SUP>-6</SUP> bar level, a significantly higher altitude than most previous results in the literature. Further ground-based observations covering other longitudes are needed to test if these mixing ratios are representative values for the equatorial and polar regions.
Kim, S.J.,Geballe, T.R.,Greathouse, T.K.,Yung, Y.L.,Miller, S.,Orton, G.S.,Minh, Y.C. Academic Press 2017 Icarus Vol.281 No.-
<P>We have derived homopause temperatures of 180-250 K for the 8-mu m north-polar hot spot (8NPHS) of Jupiter by fitting CH4 emission models to 3 and 8 mu m spectra of the 8NPHS obtained 24 days apart in 2013. From the fits, we find that CH4 mixing ratios at the 8NPHS are consistent with those reported by Kim et al. (2014) in equatorial regions. We propose possible mechanisms to account for the temperature of the 8NPHS homopause, which is relatively cool compared with the temperatures of other auroral regions, including locally-fixed and transient but energetic auroral particle precipitation. (C) 2016 Elsevier Inc. All rights reserved.</P>