Photolysis of sulphuric acid as the source of sulphur oxides in the mesosphere of Venus
Identifieur interne : 000737 ( Hal/Checkpoint ); précédent : 000736; suivant : 000738Photolysis of sulphuric acid as the source of sulphur oxides in the mesosphere of Venus
Auteurs : Xi Zhang [États-Unis] ; Mao-Chang Liang [Taïwan] ; Franck Montmessin [France] ; Jean-Loup Bertaux [France] ; Christopher Parkinson [États-Unis] ; Yuk L. Yung [États-Unis]Source :
- Nature Geoscience [ 1752-0894 ] ; 2010.
Abstract
The sulphur cycle plays fundamental roles in the chemistry and climate of Venus. Thermodynamic equilibrium chemistry at the surface of Venus favours the production of carbonyl sulphide and to a lesser extent sulphur dioxide. These gases are transported to the middle atmosphere by the Hadley circulation cell. Above the cloud top, a sulphur oxidation cycle involves conversion of carbonyl sulphide into sulphur dioxide, which is then transported further upwards. A significant fraction of this sulphur dioxide is subsequently oxidized to sulphur trioxide and eventually reacts with water to form sulphuric acid3. Because the vapour pressure of sulphuric acid is low, it readily condenses and forms an upper cloud layer at altitudes of 60-70 km, and an upper haze layer above 70 km, which effectively sequesters sulphur oxides from photochemical reactions. Here we present simulations of the fate of sulphuric acid in the Venusian mesosphere based on the Caltech/JPL kinetics model, but including the photolysis of sulphuric acid. Our model suggests that the mixing ratios of sulphur oxides are at least five times higher above 90 km when the photolysis of sulphuric acid is included. Our results are inconsistent with the previous model results but in agreement with the recent observations using ground-based microwave spectroscopy and by Venus Express.
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DOI: 10.1038/ngeo989
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Yung</name><affiliation wicri:level="1"><hal:affiliation type="laboratory" xml:id="struct-75943" status="INCOMING"> <orgName>Caltech,</orgName> <desc> <address> <addrLine>Pasadena, CA 91125</addrLine> <country key="US"></country> </address> </desc> <listRelation> <relation active="#struct-300054" type="direct"></relation> <relation active="#struct-366206" type="direct"></relation> </listRelation><tutelles><tutelle active="#struct-300054" type="direct"><org type="institution" xml:id="struct-300054" status="VALID"> <orgName>California Institute of Technology</orgName> <desc> <address> <country key="US"></country> </address> </desc></org></tutelle><tutelle active="#struct-366206" type="direct"><org type="institution" xml:id="struct-366206" status="INCOMING"> <orgName>Caltech</orgName> <desc> <address> <country key="FR"></country> </address> </desc></org></tutelle></tutelles></hal:affiliation><country>États-Unis</country></affiliation></author></analytic><idno type="DOI">10.1038/ngeo989</idno><series><title level="j">Nature Geoscience</title><idno type="ISSN">1752-0894</idno><imprint><date type="datePub">2010</date></imprint></series></biblStruct></sourceDesc></fileDesc><profileDesc><textClass></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The sulphur cycle plays fundamental roles in the chemistry and climate of Venus. Thermodynamic equilibrium chemistry at the surface of Venus favours the production of carbonyl sulphide and to a lesser extent sulphur dioxide. These gases are transported to the middle atmosphere by the Hadley circulation cell. Above the cloud top, a sulphur oxidation cycle involves conversion of carbonyl sulphide into sulphur dioxide, which is then transported further upwards. A significant fraction of this sulphur dioxide is subsequently oxidized to sulphur trioxide and eventually reacts with water to form sulphuric acid3. Because the vapour pressure of sulphuric acid is low, it readily condenses and forms an upper cloud layer at altitudes of 60-70 km, and an upper haze layer above 70 km, which effectively sequesters sulphur oxides from photochemical reactions. Here we present simulations of the fate of sulphuric acid in the Venusian mesosphere based on the Caltech/JPL kinetics model, but including the photolysis of sulphuric acid. Our model suggests that the mixing ratios of sulphur oxides are at least five times higher above 90 km when the photolysis of sulphuric acid is included. Our results are inconsistent with the previous model results but in agreement with the recent observations using ground-based microwave spectroscopy and by Venus Express.</div></front></TEI><hal api="V3"> <titleStmt> <title xml:lang="en">Photolysis of sulphuric acid as the source of sulphur oxides in the mesosphere of Venus</title> <author role="aut"> <persName> <forename type="first">Xi</forename> <surname>Zhang</surname> </persName> <idno type="halauthorid">554448</idno> <affiliation ref="#struct-75943"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Mao-Chang</forename> <surname>Liang</surname> </persName> <idno type="halauthorid">415513</idno> <affiliation ref="#struct-134874"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Franck</forename> <surname>Montmessin</surname> </persName> <idno type="halauthorid">70752</idno> <affiliation ref="#struct-391267"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Jean-Loup</forename> <surname>Bertaux</surname> </persName> <idno type="halauthorid">95580</idno> <affiliation ref="#struct-391267"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Christopher</forename> <surname>Parkinson</surname> </persName> <idno type="halauthorid">554449</idno> <affiliation ref="#struct-92830"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Yuk L.</forename> <surname>Yung</surname> </persName> <idno type="halauthorid">415514</idno> <affiliation ref="#struct-75943"></affiliation> </author> <editor role="depositor"> <persName> <forename>Catherine</forename> <surname>Cardon</surname> </persName> <email type="md5">5b4fe027ebb68973b438250ec0197c65</email> <email type="domain">noos.fr</email> </editor> </titleStmt> <editionStmt> <edition n="v1" type="current"> <date type="whenSubmitted">2010-12-06 10:08:10</date> <date type="whenModified">2017-02-09 15:53:07</date> <date type="whenReleased">2010-12-06 10:08:10</date> <date type="whenProduced">2010</date> </edition> <respStmt> <resp>contributor</resp> <name key="104093"> <persName> <forename>Catherine</forename> <surname>Cardon</surname> </persName> <email type="md5">5b4fe027ebb68973b438250ec0197c65</email> <email type="domain">noos.fr</email> </name> </respStmt> </editionStmt> <publicationStmt> <distributor>CCSD</distributor> <idno type="halId">hal-00543196</idno> <idno type="halUri">https://hal.archives-ouvertes.fr/hal-00543196</idno> <idno type="halBibtex">zhang:hal-00543196</idno> <idno type="halRefHtml">Nature Geoscience, Nature Publishing Group, 2010, 3 (12), pp.834-837. <10.1038/ngeo989></idno> <idno type="halRef">Nature Geoscience, Nature Publishing Group, 2010, 3 (12), pp.834-837. <10.1038/ngeo989></idno> </publicationStmt> <seriesStmt> <idno type="stamp" n="UPMC">Université Pierre et Marie Curie</idno> <idno type="stamp" n="INSU">INSU - Institut National des Sciences de l'Univers</idno> <idno type="stamp" n="CNRS">CNRS - Centre national de la recherche scientifique</idno> <idno type="stamp" n="LATMOS" p="UPMC">Laboratoire Atmosphères, Milieux, Observations Spatiales</idno> <idno type="stamp" n="UVSQ">Université de Versailles Saint-Quentin-en-Yvelines</idno> </seriesStmt> <notesStmt> <note type="audience" n="2">International</note> <note type="popular" n="0">No</note> <note type="peer" n="1">Yes</note> </notesStmt> <sourceDesc> <biblStruct> <analytic> <title xml:lang="en">Photolysis of sulphuric acid as the source of sulphur oxides in the mesosphere of Venus</title> <author role="aut"> <persName> <forename type="first">Xi</forename> <surname>Zhang</surname> </persName> <idno type="halauthorid">554448</idno> <affiliation ref="#struct-75943"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Mao-Chang</forename> <surname>Liang</surname> </persName> <idno type="halauthorid">415513</idno> <affiliation ref="#struct-134874"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Franck</forename> <surname>Montmessin</surname> </persName> <idno type="halauthorid">70752</idno> <affiliation ref="#struct-391267"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Jean-Loup</forename> <surname>Bertaux</surname> </persName> <idno type="halauthorid">95580</idno> <affiliation ref="#struct-391267"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Christopher</forename> <surname>Parkinson</surname> </persName> <idno type="halauthorid">554449</idno> <affiliation ref="#struct-92830"></affiliation> </author> <author role="aut"> <persName> <forename type="first">Yuk L.</forename> <surname>Yung</surname> </persName> <idno type="halauthorid">415514</idno> <affiliation ref="#struct-75943"></affiliation> </author> </analytic> <monogr> <idno type="halJournalId" status="VALID">101265</idno> <idno type="issn">1752-0894</idno> <title level="j">Nature Geoscience</title> <imprint> <publisher>Nature Publishing Group</publisher> <biblScope unit="volume">3</biblScope> <biblScope unit="issue">12</biblScope> <biblScope unit="pp">834-837</biblScope> <date type="datePub">2010</date> </imprint> </monogr> <idno type="doi">10.1038/ngeo989</idno> </biblStruct> </sourceDesc> <profileDesc> <langUsage> <language ident="en">English</language> </langUsage> <textClass> <classCode scheme="halDomain" n="sdu.astr.ep">Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]</classCode> <classCode scheme="halDomain" n="phys.astr.ep">Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]</classCode> <classCode scheme="halTypology" n="ART">Journal articles</classCode> </textClass> <abstract xml:lang="en">The sulphur cycle plays fundamental roles in the chemistry and climate of Venus. Thermodynamic equilibrium chemistry at the surface of Venus favours the production of carbonyl sulphide and to a lesser extent sulphur dioxide. These gases are transported to the middle atmosphere by the Hadley circulation cell. Above the cloud top, a sulphur oxidation cycle involves conversion of carbonyl sulphide into sulphur dioxide, which is then transported further upwards. A significant fraction of this sulphur dioxide is subsequently oxidized to sulphur trioxide and eventually reacts with water to form sulphuric acid3. Because the vapour pressure of sulphuric acid is low, it readily condenses and forms an upper cloud layer at altitudes of 60-70 km, and an upper haze layer above 70 km, which effectively sequesters sulphur oxides from photochemical reactions. Here we present simulations of the fate of sulphuric acid in the Venusian mesosphere based on the Caltech/JPL kinetics model, but including the photolysis of sulphuric acid. Our model suggests that the mixing ratios of sulphur oxides are at least five times higher above 90 km when the photolysis of sulphuric acid is included. Our results are inconsistent with the previous model results but in agreement with the recent observations using ground-based microwave spectroscopy and by Venus Express.</abstract> </profileDesc> </hal></record>Pour manipuler ce document sous Unix (Dilib)
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