Saturn's Stratospheric Acetylene And Ethane Emission

Brigette E. Hesman; D. E. Jennings; P. V. Sada; G. L. Bjoraker; A. A. Simon-Miller; C. A. Nixon; R. J. Boyle; G. H. McCabe

Saturn's Stratospheric Acetylene And Ethane Emission

Brigette E. Hesman, D. E. Jennings, P. V. Sada, G. L. Bjoraker, A. A. Simon-Miller, C. A. Nixon, R. J. Boyle, G. H. McCabe

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Abstract

Hydrocarbons in the upper atmosphere of Saturn are known, from Voyager and early Cassini results, to vary in emission intensity with latitude. Of particular interest is the marked increase in temperature and hydrocarbon line intensity near the South Pole (Greathouse et al. 2005, Orton and Yanamandra-Fisher, 2005, Flasar et al. 2005). Latitudinal variations in hydrocarbon abundances can be determined from measurements of hydrocarbon emission lines using temperatures derived from Cassini’s Composite InfRared Spectrometer (CIRS). Latitudinal, temporal, and vertical variations of stratospheric hydrocarbons provide constraints on dynamics, seasonal climate models, and photochemical models. In an effort to monitor temporal and latitudinal variations of hydrocarbons in Saturn’s southern hemisphere we are conducting a ground-based campaign using Celeste, an infrared (5-25 μm) high-resolution (

Original language	English
Journal	American Astronomical Society Meeting 210
Volume	210
Publication status	Published - 1 May 2007
Externally published	Yes

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http://adsabs.harvard.edu/abs/2007AAS...210.8901H

Cite this

@article{23622ecd82be4b699c41a9d66485da9c,

title = "Saturn's Stratospheric Acetylene And Ethane Emission",

abstract = "Hydrocarbons in the upper atmosphere of Saturn are known, from Voyager and early Cassini results, to vary in emission intensity with latitude. Of particular interest is the marked increase in temperature and hydrocarbon line intensity near the South Pole (Greathouse et al. 2005, Orton and Yanamandra-Fisher, 2005, Flasar et al. 2005). Latitudinal variations in hydrocarbon abundances can be determined from measurements of hydrocarbon emission lines using temperatures derived from Cassini{\textquoteright}s Composite InfRared Spectrometer (CIRS). Latitudinal, temporal, and vertical variations of stratospheric hydrocarbons provide constraints on dynamics, seasonal climate models, and photochemical models. In an effort to monitor temporal and latitudinal variations of hydrocarbons in Saturn{\textquoteright}s southern hemisphere we are conducting a ground-based campaign using Celeste, an infrared (5-25 μm) high-resolution (",

author = "Hesman, {Brigette E.} and Jennings, {D. E.} and Sada, {P. V.} and Bjoraker, {G. L.} and Simon-Miller, {A. A.} and Nixon, {C. A.} and Boyle, {R. J.} and McCabe, {G. H.}",

year = "2007",

month = may,

day = "1",

language = "English",

volume = "210",

journal = "American Astronomical Society Meeting 210",

}

TY - JOUR

T1 - Saturn's Stratospheric Acetylene And Ethane Emission

AU - Hesman, Brigette E.

AU - Jennings, D. E.

AU - Sada, P. V.

AU - Bjoraker, G. L.

AU - Simon-Miller, A. A.

AU - Nixon, C. A.

AU - Boyle, R. J.

AU - McCabe, G. H.

PY - 2007/5/1

Y1 - 2007/5/1

N2 - Hydrocarbons in the upper atmosphere of Saturn are known, from Voyager and early Cassini results, to vary in emission intensity with latitude. Of particular interest is the marked increase in temperature and hydrocarbon line intensity near the South Pole (Greathouse et al. 2005, Orton and Yanamandra-Fisher, 2005, Flasar et al. 2005). Latitudinal variations in hydrocarbon abundances can be determined from measurements of hydrocarbon emission lines using temperatures derived from Cassini’s Composite InfRared Spectrometer (CIRS). Latitudinal, temporal, and vertical variations of stratospheric hydrocarbons provide constraints on dynamics, seasonal climate models, and photochemical models. In an effort to monitor temporal and latitudinal variations of hydrocarbons in Saturn’s southern hemisphere we are conducting a ground-based campaign using Celeste, an infrared (5-25 μm) high-resolution (

AB - Hydrocarbons in the upper atmosphere of Saturn are known, from Voyager and early Cassini results, to vary in emission intensity with latitude. Of particular interest is the marked increase in temperature and hydrocarbon line intensity near the South Pole (Greathouse et al. 2005, Orton and Yanamandra-Fisher, 2005, Flasar et al. 2005). Latitudinal variations in hydrocarbon abundances can be determined from measurements of hydrocarbon emission lines using temperatures derived from Cassini’s Composite InfRared Spectrometer (CIRS). Latitudinal, temporal, and vertical variations of stratospheric hydrocarbons provide constraints on dynamics, seasonal climate models, and photochemical models. In an effort to monitor temporal and latitudinal variations of hydrocarbons in Saturn’s southern hemisphere we are conducting a ground-based campaign using Celeste, an infrared (5-25 μm) high-resolution (

M3 - Article

VL - 210

JO - American Astronomical Society Meeting 210

JF - American Astronomical Society Meeting 210

ER -

Saturn's Stratospheric Acetylene And Ethane Emission

Abstract

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