Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini
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, CH and CH, retrieved from the Cassini and Voyager observations in the latitude and vertical plane, with a careful error analysis. The non-LTE effect i...
| Main Authors: | , , , , , , , |
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| Format: | Journal article |
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2013
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| _version_ | 1797097331511787520 |
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| author | Zhang, X Nixon, C Shia, R West, R Irwin, P Yelle, R Allen, M Yung, Y |
| author_facet | Zhang, X Nixon, C Shia, R West, R Irwin, P Yelle, R Allen, M Yung, Y |
| author_sort | Zhang, X |
| collection | OXFORD |
| description | 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, CH and CH, 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 (CH), acetylene (CH) and methane (CH), in the region above. The two-dimensional cooling rate maps are influenced primarily by the temperature structure, and also by the meridional distributions of CH and CH. The temperature anomalies at the 1 mbar pressure level in the Cassini data and the strong CH 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 CH 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. © 2013 Elsevier Ltd. |
| first_indexed | 2024-03-07T04:54:00Z |
| format | Journal article |
| id | oxford-uuid:d5f5a9aa-18d4-4edb-829b-8dfabffee4d1 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T04:54:00Z |
| publishDate | 2013 |
| record_format | dspace |
| spelling | oxford-uuid:d5f5a9aa-18d4-4edb-829b-8dfabffee4d12022-03-27T08:29:49ZRadiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to CassiniJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:d5f5a9aa-18d4-4edb-829b-8dfabffee4d1Symplectic Elements at Oxford2013Zhang, XNixon, CShia, RWest, RIrwin, PYelle, RAllen, MYung, YWe 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, CH and CH, 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 (CH), acetylene (CH) and methane (CH), in the region above. The two-dimensional cooling rate maps are influenced primarily by the temperature structure, and also by the meridional distributions of CH and CH. The temperature anomalies at the 1 mbar pressure level in the Cassini data and the strong CH 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 CH 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. © 2013 Elsevier Ltd. |
| spellingShingle | Zhang, X Nixon, C Shia, R West, R Irwin, P Yelle, R Allen, M Yung, Y Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini |
| title | Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini |
| title_full | Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini |
| title_fullStr | Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini |
| title_full_unstemmed | Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini |
| title_short | Radiative forcing of the stratosphere of Jupiter, Part I: Atmospheric cooling rates from Voyager to Cassini |
| title_sort | radiative forcing of the stratosphere of jupiter part i atmospheric cooling rates from voyager to cassini |
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