Temporally varying ethylene emission on Jupiter

Paul N. Romani, Donald E. Jennings, Gordon L. Bjoraker, Pedro V. Sada, George H. McCabe, Robert J. Boyle

Research output: Contribution to journalArticle

22 Citations (Scopus)

Abstract

Ethylene (C 2H 4) emission has been measured in the poles and equator of Jupiter. The 949 cm -1 spectra were recorded with a high resolution spectrometer at the McMath-Pierce telescope at Kitt Peak in October-November 1998 and at the Infrared Telescope Facility at Mauna Kea in June 2000. C 2H 4 is an important product of methane chemistry in the outer planets. Knowledge of its abundance can help discriminate among the various proposed sets of CH 4 photolysis branching ratios at Ly- α, and determine the relative importance of the reaction pathways that produce C 2H 2 and C 2H 6. In the equatorial region the C 2H 4 emission is weak, and we were only able to detect it at high air-mass, near the limb. We derive a peak equatorial molar abundance of C 2H 4 of 4.5×10-1.7×10 near 2.2×10 mbar, with a total column of 5.7×10-2.2×10 molecules cm -2 above 10 mbar depending upon choice of thermal profile. We observed enhanced C 2H 4 emission from the poles in the regions where auroras are seen in X-ray, UV, and near infrared images. In 2000 we measured a short-term change in the distribution of polar C 2H 4 emission; the emission in the north IR auroral "hot spot" decreased by a factor of three over a two-day interval. This transient behavior and the sensitivity of C 2H 4 emission to temperature changes near its contribution peak at 5-10 microbar suggests that the polar enhancement is primarily a thermal effect coupled with vertical transport. Comparing our observations from Kitt Peak and Mauna Kea shows that the C 2H 4 emission of the northern non-"hot spot" auroral regions did not change over the three-year period while that in the southern polar regions decreased.
Original languageEnglish
Pages (from-to)420-434
JournalIcarus
Volume198
Issue number2
DOIs
Publication statusPublished - 1 Dec 2008
Externally publishedYes

Fingerprint

Jupiter (planet)
Jupiter
ethylene
poles
auroras
equatorial regions
air masses
equators
photolysis
polar region
limbs
temperature effect
polar regions
air mass
temperature effects
limb
near infrared
spectrometer
methane
spectrometers

Cite this

Romani, P. N., Jennings, D. E., Bjoraker, G. L., Sada, P. V., McCabe, G. H., & Boyle, R. J. (2008). Temporally varying ethylene emission on Jupiter. Icarus, 198(2), 420-434. https://doi.org/10.1016/j.icarus.2008.05.027
Romani, Paul N. ; Jennings, Donald E. ; Bjoraker, Gordon L. ; Sada, Pedro V. ; McCabe, George H. ; Boyle, Robert J. / Temporally varying ethylene emission on Jupiter. In: Icarus. 2008 ; Vol. 198, No. 2. pp. 420-434.
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abstract = "Ethylene (C 2H 4) emission has been measured in the poles and equator of Jupiter. The 949 cm -1 spectra were recorded with a high resolution spectrometer at the McMath-Pierce telescope at Kitt Peak in October-November 1998 and at the Infrared Telescope Facility at Mauna Kea in June 2000. C 2H 4 is an important product of methane chemistry in the outer planets. Knowledge of its abundance can help discriminate among the various proposed sets of CH 4 photolysis branching ratios at Ly- α, and determine the relative importance of the reaction pathways that produce C 2H 2 and C 2H 6. In the equatorial region the C 2H 4 emission is weak, and we were only able to detect it at high air-mass, near the limb. We derive a peak equatorial molar abundance of C 2H 4 of 4.5×10-1.7×10 near 2.2×10 mbar, with a total column of 5.7×10-2.2×10 molecules cm -2 above 10 mbar depending upon choice of thermal profile. We observed enhanced C 2H 4 emission from the poles in the regions where auroras are seen in X-ray, UV, and near infrared images. In 2000 we measured a short-term change in the distribution of polar C 2H 4 emission; the emission in the north IR auroral {"}hot spot{"} decreased by a factor of three over a two-day interval. This transient behavior and the sensitivity of C 2H 4 emission to temperature changes near its contribution peak at 5-10 microbar suggests that the polar enhancement is primarily a thermal effect coupled with vertical transport. Comparing our observations from Kitt Peak and Mauna Kea shows that the C 2H 4 emission of the northern non-{"}hot spot{"} auroral regions did not change over the three-year period while that in the southern polar regions decreased.",
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Romani, PN, Jennings, DE, Bjoraker, GL, Sada, PV, McCabe, GH & Boyle, RJ 2008, 'Temporally varying ethylene emission on Jupiter', Icarus, vol. 198, no. 2, pp. 420-434. https://doi.org/10.1016/j.icarus.2008.05.027

Temporally varying ethylene emission on Jupiter. / Romani, Paul N.; Jennings, Donald E.; Bjoraker, Gordon L.; Sada, Pedro V.; McCabe, George H.; Boyle, Robert J.

In: Icarus, Vol. 198, No. 2, 01.12.2008, p. 420-434.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Temporally varying ethylene emission on Jupiter

AU - Romani, Paul N.

AU - Jennings, Donald E.

AU - Bjoraker, Gordon L.

AU - Sada, Pedro V.

AU - McCabe, George H.

AU - Boyle, Robert J.

PY - 2008/12/1

Y1 - 2008/12/1

N2 - Ethylene (C 2H 4) emission has been measured in the poles and equator of Jupiter. The 949 cm -1 spectra were recorded with a high resolution spectrometer at the McMath-Pierce telescope at Kitt Peak in October-November 1998 and at the Infrared Telescope Facility at Mauna Kea in June 2000. C 2H 4 is an important product of methane chemistry in the outer planets. Knowledge of its abundance can help discriminate among the various proposed sets of CH 4 photolysis branching ratios at Ly- α, and determine the relative importance of the reaction pathways that produce C 2H 2 and C 2H 6. In the equatorial region the C 2H 4 emission is weak, and we were only able to detect it at high air-mass, near the limb. We derive a peak equatorial molar abundance of C 2H 4 of 4.5×10-1.7×10 near 2.2×10 mbar, with a total column of 5.7×10-2.2×10 molecules cm -2 above 10 mbar depending upon choice of thermal profile. We observed enhanced C 2H 4 emission from the poles in the regions where auroras are seen in X-ray, UV, and near infrared images. In 2000 we measured a short-term change in the distribution of polar C 2H 4 emission; the emission in the north IR auroral "hot spot" decreased by a factor of three over a two-day interval. This transient behavior and the sensitivity of C 2H 4 emission to temperature changes near its contribution peak at 5-10 microbar suggests that the polar enhancement is primarily a thermal effect coupled with vertical transport. Comparing our observations from Kitt Peak and Mauna Kea shows that the C 2H 4 emission of the northern non-"hot spot" auroral regions did not change over the three-year period while that in the southern polar regions decreased.

AB - Ethylene (C 2H 4) emission has been measured in the poles and equator of Jupiter. The 949 cm -1 spectra were recorded with a high resolution spectrometer at the McMath-Pierce telescope at Kitt Peak in October-November 1998 and at the Infrared Telescope Facility at Mauna Kea in June 2000. C 2H 4 is an important product of methane chemistry in the outer planets. Knowledge of its abundance can help discriminate among the various proposed sets of CH 4 photolysis branching ratios at Ly- α, and determine the relative importance of the reaction pathways that produce C 2H 2 and C 2H 6. In the equatorial region the C 2H 4 emission is weak, and we were only able to detect it at high air-mass, near the limb. We derive a peak equatorial molar abundance of C 2H 4 of 4.5×10-1.7×10 near 2.2×10 mbar, with a total column of 5.7×10-2.2×10 molecules cm -2 above 10 mbar depending upon choice of thermal profile. We observed enhanced C 2H 4 emission from the poles in the regions where auroras are seen in X-ray, UV, and near infrared images. In 2000 we measured a short-term change in the distribution of polar C 2H 4 emission; the emission in the north IR auroral "hot spot" decreased by a factor of three over a two-day interval. This transient behavior and the sensitivity of C 2H 4 emission to temperature changes near its contribution peak at 5-10 microbar suggests that the polar enhancement is primarily a thermal effect coupled with vertical transport. Comparing our observations from Kitt Peak and Mauna Kea shows that the C 2H 4 emission of the northern non-"hot spot" auroral regions did not change over the three-year period while that in the southern polar regions decreased.

U2 - 10.1016/j.icarus.2008.05.027

DO - 10.1016/j.icarus.2008.05.027

M3 - Article

VL - 198

SP - 420

EP - 434

JO - Icarus

JF - Icarus

SN - 0019-1035

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ER -

Romani PN, Jennings DE, Bjoraker GL, Sada PV, McCabe GH, Boyle RJ. Temporally varying ethylene emission on Jupiter. Icarus. 2008 Dec 1;198(2):420-434. https://doi.org/10.1016/j.icarus.2008.05.027