High-resolution spectroscopy of Saturn at 3 microns: CH4, CH3D, C2H2, C2H6, PH3, clouds, and haze

Kim, Joo Hyeon; Kim, Sang J.; Geballe, T. R.; Kim, Sungsoo S.; Brown, Linda R.

doi:10.1016/j.icarus.2006.07.004

Cited by 33 publications

(28 citation statements)

References 34 publications

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“…[ Kim et al (2006), centered at 40°S. They determined the C 2 H 6 abundance using its ν 7 emission band at 3.3 µm to be 9±4 × 10 (a mean of the abundances from 35°S to 45°S).…”

Section: Ethanementioning

confidence: 99%

Vertical and meridional distribution of ethane, acetylene and propane in Saturn’s stratosphere from CIRS/Cassini limb observations

Guerlet¹,

Fouchet²,

Bézard³

et al. 2009

Icarus

200

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“…[ Kim et al (2006), centered at 40°S. They determined the C 2 H 6 abundance using its ν 7 emission band at 3.3 µm to be 9±4 × 10 (a mean of the abundances from 35°S to 45°S).…”

Section: Ethanementioning

confidence: 99%

Vertical and meridional distribution of ethane, acetylene and propane in Saturn’s stratosphere from CIRS/Cassini limb observations

Guerlet¹,

Fouchet²,

Bézard³

et al. 2009

Icarus

200

View full text Add to dashboard Cite

“…For approximating the CH 4 , C 2 H 2 , and C 2 H 6 emission bands in our synthetic spectra we used a modified version of the radiative transfer program used for Saturn by Kim et al (2006). For the line positions, intensities, widths, and ground state energies of all three species we adopted the values previously used for Saturn (Kim et al, 2006).…”

Section: Radiative Cooling Ratesmentioning

confidence: 99%

Jupiter's hydrocarbon polar brightening: Discovery of 3-micron line emission from south polar CH4, C2H2, and C2H6

Kim¹,

Geballe²,

Seo³

et al. 2009

Icarus

Self Cite

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“…The middle atmospheres of Jupiter and Saturn are characterized by various aerosols, hazes and multiple cloud layers that scatter visible radiation and limit its penetration to the lower atmospheres (e.g., Atreya et al 1999;Moses 2000;West et al 2004;Kim et al 2006). Although NH 3 is an important minor component of the lower atmospheres of these planets (e.g., de Pater and Massie 1985;de Pater and Lissauer 2001), ammonia and NH 4 SH condense to form cloud layers in the tropospheres of Jupiter and on Saturn.…”

Section: Photoabsorption and Scattering Of Visible Photonsmentioning

confidence: 99%

“…Although NH 3 is an important minor component of the lower atmospheres of these planets (e.g., de Pater and Massie 1985;de Pater and Lissauer 2001), ammonia and NH 4 SH condense to form cloud layers in the tropospheres of Jupiter and on Saturn. At higher altitudes, in the stratospheres of these planets, hydrocarbon haze layers are also present (e.g., Moses 2000;Kim et al 2006). In the colder atmospheres of Uranus and Neptune, photochemical hydrocarbon hazes and ices may form in the stratospheres (e.g., Moses et al 1992), and methane ices probably form tropospheric clouds (e.g., Baines et al 1995).…”

Section: Photoabsorption and Scattering Of Visible Photonsmentioning

confidence: 99%

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

2008

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We discuss here the energy deposition of solar FUV, EUV and X-ray photons, energetic auroral particles, and pickup ions. Photons and the photoelectrons that they produce may interact with thermospheric neutral species producing dissociation, ionization, excitation, and heating. The interaction of X-rays or keV electrons with atmospheric neutrals may produce core-ionized species, which may decay by the production of characteristic X-rays or Auger electrons. Energetic particles may precipitate into the atmosphere, and their collisions with atmospheric particles also produce ionization, excitation, and heating, and auroral emissions. Auroral energetic particles, like photoelectrons, interact with the atmospheric species through discrete collisions that produce ionization, excitation, and heating of the ambient electron population. Auroral particles are, however, not restricted to the sunlit regions. They originate outside the atmosphere and are more energetic than photoelectrons, especially at magnetized planets. The spectroscopic analysis of auroral emissions is discussed here, along with its relevance to precipitating particle diagnostics. Atmospheres can also be modified by the energy deposited by the incident pickup ions with energies of eV's to MeV's; these particles may be of solar wind origin, or from a magnetospheric plasma. When the modeling of the energy deposition of the plasma is calculated, the subsequent modeling of the atmospheric processes, such as chemistry, emission, and the fate of hot recoil particles produced is roughly independent of the exciting radiation. However, calculating the spatial distribution of the energy deposition versus depth into the atmosphere produced by an incident plasma is much more complex than is the calculation of the solar excitation profile. Here, the nature of the energy deposition processes by the incident plasma are described as is the fate of the hot recoil particles produced by exothermic chemistry and by knock-on collisions by the incident ions.

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High-resolution spectroscopy of Saturn at 3 microns: CH4, CH3D, C2H2, C2H6, PH3, clouds, and haze

Cited by 33 publications

References 34 publications

Vertical and meridional distribution of ethane, acetylene and propane in Saturn’s stratosphere from CIRS/Cassini limb observations

Vertical and meridional distribution of ethane, acetylene and propane in Saturn’s stratosphere from CIRS/Cassini limb observations

Jupiter's hydrocarbon polar brightening: Discovery of 3-micron line emission from south polar CH4, C2H2, and C2H6

Energy Deposition in Planetary Atmospheres by Charged Particles and Solar Photons

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