Abstract
We developed a line-by-line heating and cooling rate model for the stratosphere of Jupiter, based on two complete sets of global maps of temperature, C2H2 and C2H6, retrieved from the Cassini and Voyager observations in the latitude and vertical plane, with a careful error analysis. The non-LTE effect is found unimportant on the thermal cooling rate below the 0.01 mbar pressure level. The most important coolants are molecular hydrogen between 10 and 100 mbar, and hydrocarbons, including ethane (C2H6), acetylene (C2H2)and methane(CH4), in the region above. The two-dimensional cooling rate maps are influenced primarily by the temperature structure, and also by the meridional distributions of C2H2 and C2H6.The temperature anomalies at the 1 mbar pressure level in the Cassini data and the strong C2H6 latitudinal contrast in the Voyager epoch are the two most prominent features influencing the cooling rate patterns, with the effect from the 'quasi-quadrennial oscillation (QQO)' thermal structures at ~20 mbar. The globally averaged CH4 heating and cooling rates are not balanced, clearly in the lower stratosphere under 10 mbar, and possibly in the upper stratosphere above the 1 mbar pressure level. Possible heating sources from the gravity wave breaking and aerosols are discussed. The radiative relaxation timescale in the lower stratosphere implies that the temperature profile might not be purely radiatively controlled.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 3-25 |
| Number of pages | 23 |
| Journal | Planetary and Space Science |
| Volume | 88 |
| DOIs | |
| State | Published - 2013 |
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Keywords
- Abundance retrieval
- Energy balance
- Jupiter atmosphere
- Outer planets
- Radiative transfer
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
Cite this
Radiative forcing of the stratosphere of Jupiter, Part I : Atmospheric cooling rates from Voyager to Cassini. / Zhang, X.; Nixon, C. A.; Shia, R. L.; West, R. A.; Irwin, P. G J; Yelle, Roger; Allen, M. A.; Yung, Y. L.
In: Planetary and Space Science, Vol. 88, 2013, p. 3-25.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Radiative forcing of the stratosphere of Jupiter, Part I
T2 - Atmospheric cooling rates from Voyager to Cassini
AU - Zhang, X.
AU - Nixon, C. A.
AU - Shia, R. L.
AU - West, R. A.
AU - Irwin, P. G J
AU - Yelle, Roger
AU - Allen, M. A.
AU - Yung, Y. L.
PY - 2013
Y1 - 2013
N2 - We developed a line-by-line heating and cooling rate model for the stratosphere of Jupiter, based on two complete sets of global maps of temperature, C2H2 and C2H6, retrieved from the Cassini and Voyager observations in the latitude and vertical plane, with a careful error analysis. The non-LTE effect is found unimportant on the thermal cooling rate below the 0.01 mbar pressure level. The most important coolants are molecular hydrogen between 10 and 100 mbar, and hydrocarbons, including ethane (C2H6), acetylene (C2H2)and methane(CH4), in the region above. The two-dimensional cooling rate maps are influenced primarily by the temperature structure, and also by the meridional distributions of C2H2 and C2H6.The temperature anomalies at the 1 mbar pressure level in the Cassini data and the strong C2H6 latitudinal contrast in the Voyager epoch are the two most prominent features influencing the cooling rate patterns, with the effect from the 'quasi-quadrennial oscillation (QQO)' thermal structures at ~20 mbar. The globally averaged CH4 heating and cooling rates are not balanced, clearly in the lower stratosphere under 10 mbar, and possibly in the upper stratosphere above the 1 mbar pressure level. Possible heating sources from the gravity wave breaking and aerosols are discussed. The radiative relaxation timescale in the lower stratosphere implies that the temperature profile might not be purely radiatively controlled.
AB - We developed a line-by-line heating and cooling rate model for the stratosphere of Jupiter, based on two complete sets of global maps of temperature, C2H2 and C2H6, retrieved from the Cassini and Voyager observations in the latitude and vertical plane, with a careful error analysis. The non-LTE effect is found unimportant on the thermal cooling rate below the 0.01 mbar pressure level. The most important coolants are molecular hydrogen between 10 and 100 mbar, and hydrocarbons, including ethane (C2H6), acetylene (C2H2)and methane(CH4), in the region above. The two-dimensional cooling rate maps are influenced primarily by the temperature structure, and also by the meridional distributions of C2H2 and C2H6.The temperature anomalies at the 1 mbar pressure level in the Cassini data and the strong C2H6 latitudinal contrast in the Voyager epoch are the two most prominent features influencing the cooling rate patterns, with the effect from the 'quasi-quadrennial oscillation (QQO)' thermal structures at ~20 mbar. The globally averaged CH4 heating and cooling rates are not balanced, clearly in the lower stratosphere under 10 mbar, and possibly in the upper stratosphere above the 1 mbar pressure level. Possible heating sources from the gravity wave breaking and aerosols are discussed. The radiative relaxation timescale in the lower stratosphere implies that the temperature profile might not be purely radiatively controlled.
KW - Abundance retrieval
KW - Energy balance
KW - Jupiter atmosphere
KW - Outer planets
KW - Radiative transfer
UR - http://www.scopus.com/inward/record.url?scp=84901851986&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84901851986&partnerID=8YFLogxK
U2 - 10.1016/j.pss.2013.07.005
DO - 10.1016/j.pss.2013.07.005
M3 - Article
VL - 88
SP - 3
EP - 25
JO - Planetary and Space Science
JF - Planetary and Space Science
SN - 0032-0633
ER -