Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI
Detection of HCl on Jupiter would provide insight into the chlorine cycle and external elemental fluxes on giant planets, yet so far has not been possible. Here we present the most sensitive search for Jupiters stratospheric HCl to date using observations of the 625.907 and 1876.221 GHz spectral lin...
| Main Authors: | , , , |
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| Format: | Journal article |
| Language: | English |
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Elsevier
2014
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| _version_ | 1826260083098517504 |
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| author | Teanby, N Showman, A Fletcher, L Irwin, P |
| author_facet | Teanby, N Showman, A Fletcher, L Irwin, P |
| author_sort | Teanby, N |
| collection | OXFORD |
| description | Detection of HCl on Jupiter would provide insight into the chlorine cycle and external elemental fluxes on giant planets, yet so far has not been possible. Here we present the most sensitive search for Jupiters stratospheric HCl to date using observations of the 625.907 and 1876.221 GHz spectral lines with Herschels HIFI instrument. HCl was not detected, but we determined the most stringent upper limits so far, improving on previous studies by two orders of magnitude. If HCl is assumed to be uniformly mixed, with a constant volume mixing ratio above the 1 mbar pressure level and has zero abundance below, we obtain a 3-σ upper limit of 0.061 ppb; in contrast, if we assume uniform mixing above the 1 mbar level and allow a non-zero but downward-decreasing abundance from 1 mbar to the troposphere based on eddy diffusion, we obtain a 3-σ upper limit of 0.027 ppb. This is below the abundance expected for a solar composition cometary source and implies that upper stratospheric HCl loss processes are required for consistency with observations of the external oxygen flux. We investigated loss via aerosol scavenging using a simple diffusion model and conclude that it could be a very effective mechanism for HCl removal. Transient scavenging by stratospheric NH3 from impacts is another potentially important loss mechanism. This suggests that it is extremely unlikely that HCl is present in sufficient quantities to be detectable in the near future. An alternative explanation for our very low upper limits could be that HCl is sub-solar in comets or that cometary chlorine exists in inactive reservoirs that are not readily converted to HCl during the impact process. |
| first_indexed | 2024-03-06T18:59:59Z |
| format | Journal article |
| id | oxford-uuid:133319cd-821f-45a7-92d8-c27d46ddfe50 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T18:59:59Z |
| publishDate | 2014 |
| publisher | Elsevier |
| record_format | dspace |
| spelling | oxford-uuid:133319cd-821f-45a7-92d8-c27d46ddfe502022-03-26T10:12:26ZConstraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFIJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:133319cd-821f-45a7-92d8-c27d46ddfe50EnglishSymplectic Elements at OxfordElsevier2014Teanby, NShowman, AFletcher, LIrwin, PDetection of HCl on Jupiter would provide insight into the chlorine cycle and external elemental fluxes on giant planets, yet so far has not been possible. Here we present the most sensitive search for Jupiters stratospheric HCl to date using observations of the 625.907 and 1876.221 GHz spectral lines with Herschels HIFI instrument. HCl was not detected, but we determined the most stringent upper limits so far, improving on previous studies by two orders of magnitude. If HCl is assumed to be uniformly mixed, with a constant volume mixing ratio above the 1 mbar pressure level and has zero abundance below, we obtain a 3-σ upper limit of 0.061 ppb; in contrast, if we assume uniform mixing above the 1 mbar level and allow a non-zero but downward-decreasing abundance from 1 mbar to the troposphere based on eddy diffusion, we obtain a 3-σ upper limit of 0.027 ppb. This is below the abundance expected for a solar composition cometary source and implies that upper stratospheric HCl loss processes are required for consistency with observations of the external oxygen flux. We investigated loss via aerosol scavenging using a simple diffusion model and conclude that it could be a very effective mechanism for HCl removal. Transient scavenging by stratospheric NH3 from impacts is another potentially important loss mechanism. This suggests that it is extremely unlikely that HCl is present in sufficient quantities to be detectable in the near future. An alternative explanation for our very low upper limits could be that HCl is sub-solar in comets or that cometary chlorine exists in inactive reservoirs that are not readily converted to HCl during the impact process. |
| spellingShingle | Teanby, N Showman, A Fletcher, L Irwin, P Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI |
| title | Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI |
| title_full | Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI |
| title_fullStr | Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI |
| title_full_unstemmed | Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI |
| title_short | Constraints on Jupiter's stratospheric HCl abundance and chlorine cycle from Herschel/HIFI |
| title_sort | constraints on jupiter s stratospheric hcl abundance and chlorine cycle from herschel hifi |
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