Infrared polar brightening on Jupiter: III. Spectrometry from the Voyager 1 IRIS experiment
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Cited by (136)
Jupiter's auroral-related stratospheric heating and chemistry III: Abundances of C <inf>2</inf> H <inf>4</inf> , CH <inf>3</inf> C <inf>2</inf> H, C <inf>4</inf> H <inf>2</inf> and C <inf>6</inf> H <inf>6</inf> from Voyager-IRIS and Cassini-CIRS
2019, IcarusCitation Excerpt :High-energy ions and electrons from the Jovian magnetosphere and solar wind are injected into the neutral atmosphere and deposit their energy at pressures as deep as the 1-mbar level (Flasar et al., 2004), or approximately 175 km above the 1-bar level. The resulting charged particle precipitation, ion drag and Joule heating exemplify processes that warm the stratosphere and mesosphere, thereby enhancing the mid-infrared emission features of stratospheric species such as CH4 (methane), C2H2 (acetylene),C2H4 (ethylene) and C2H6 (Caldwell et al., 1980; Caldwell et al., 1983; Drossart et al., 1993; Kim et al., 1985; Kostiuk et al., 1993; Livengood et al., 1993). The increased flux of electrons in the auroral regions also drives increased rates of ion-neutral and electron-recombination reactions, thereby modifying the chemistry in the auroral regions with respect to non-auroral regions and lower latitudes (Sinclair et al., 2017b; Sinclair et al., 2018).
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Present address: National Space Science Data Center, Code 633, Goddard Space Flight Center, Greenbelt, Md. 20771.