Estimates of atomic deuterium abundance and Lyman‐alpha airglow in the thermosphere of Jupiter
Identifieur interne : 000313 ( France/Analysis ); précédent : 000312; suivant : 000314Estimates of atomic deuterium abundance and Lyman‐alpha airglow in the thermosphere of Jupiter
Auteurs : C. D. Parkinson [Canada] ; E. Griffioen [Canada] ; J. C. Mcconnell [Canada] ; L. Ben Jaffel [États-Unis] ; A. Vidal-Madjar [France] ; J. T. Clarke [États-Unis] ; G. R. Gladstone [États-Unis]Source :
- Geophysical Research Letters [ 0094-8276 ] ; 1999-10-15.
Abstract
We have made calculations of the atomic D distribution in the thermosphere of Jupiter. The principal reactions determining the D abundance appear to be generation by reaction of H with vibrationally hot HD and loss by reaction of D with H2(υ=0,1) and CH3. The H and CH3 distributions have been calculated using a 1‐D photochemical‐diffusion model with the column H constrained using the Lyman‐α airglow. For H2 effective vibrational temperatures, Tυ, between 1 and 4 times kinetic we find D columns between 4×1011 and 2×1013 atoms cm−2. HD can be vibrationally excited due to VV energy transfer from H2(υ=1). Using a radiative transfer model with coupling of the H and D Lyman‐α lines we have calculated line profiles and total intensities across the Jovian disk and on the limb. For the above D columns and a H column ∼3.5×1017 cm−2, compatible with equatorial Lyman‐α airglow observations, the disk D intensity varies from 80 to 600 R for overhead Sun and viewing, whereas on the terminator the D maximum total intensity is ∼60 R at ∼860 km above the 1 bar level for the maximum D column.
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DOI: 10.1029/1999GL003650
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D." last="Parkinson">C. D. Parkinson</name><affiliation wicri:level="1"><country xml:lang="fr">Canada</country><wicri:regionArea>Dept. Earth and Atmos. Sci., York University</wicri:regionArea><wicri:noRegion>York University</wicri:noRegion></affiliation></author><author><name sortKey="Griffioen, E" sort="Griffioen, E" uniqKey="Griffioen E" first="E." last="Griffioen">E. Griffioen</name><affiliation wicri:level="1"><country xml:lang="fr">Canada</country><wicri:regionArea>Dept. Earth and Atmos. Sci., York University</wicri:regionArea><wicri:noRegion>York University</wicri:noRegion></affiliation></author><author><name sortKey="Mcconnell, J C" sort="Mcconnell, J C" uniqKey="Mcconnell J" first="J. C." last="Mcconnell">J. C. Mcconnell</name><affiliation wicri:level="1"><country xml:lang="fr">Canada</country><wicri:regionArea>Dept. Earth and Atmos. Sci., York University</wicri:regionArea><wicri:noRegion>York University</wicri:noRegion></affiliation></author><author><name sortKey="Ben Jaffel, L" sort="Ben Jaffel, L" uniqKey="Ben Jaffel L" first="L." last="Ben Jaffel">L. Ben Jaffel</name><affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country><placeName><region type="state">Michigan</region></placeName><wicri:cityArea>Space Physics Research Laboratory, Ann Arbor</wicri:cityArea></affiliation></author><author><name sortKey="Vidal Adjar, A" sort="Vidal Adjar, A" uniqKey="Vidal Adjar A" first="A." last="Vidal-Madjar">A. Vidal-Madjar</name><affiliation wicri:level="1"><country xml:lang="fr">France</country><wicri:regionArea>Institut d'Astrophysique de Paris</wicri:regionArea></affiliation></author><author><name sortKey="Clarke, J T" sort="Clarke, J T" uniqKey="Clarke J" first="J. T." last="Clarke">J. T. 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Lett.</title><idno type="ISSN">0094-8276</idno><idno type="eISSN">1944-8007</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><date type="published" when="1999-10-15">1999-10-15</date><biblScope unit="volume">26</biblScope><biblScope unit="issue">20</biblScope><biblScope unit="page" from="3177">3177</biblScope><biblScope unit="page" to="3180">3180</biblScope></imprint><idno type="ISSN">0094-8276</idno></series><idno type="istex">49F2AECBA873C60E40766D5EA9F5CB1A9EF55E7A</idno><idno type="DOI">10.1029/1999GL003650</idno><idno type="ArticleID">1999GL003650</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0094-8276</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract">We have made calculations of the atomic D distribution in the thermosphere of Jupiter. The principal reactions determining the D abundance appear to be generation by reaction of H with vibrationally hot HD and loss by reaction of D with H2(υ=0,1) and CH3. The H and CH3 distributions have been calculated using a 1‐D photochemical‐diffusion model with the column H constrained using the Lyman‐α airglow. For H2 effective vibrational temperatures, Tυ, between 1 and 4 times kinetic we find D columns between 4×1011 and 2×1013 atoms cm−2. HD can be vibrationally excited due to VV energy transfer from H2(υ=1). Using a radiative transfer model with coupling of the H and D Lyman‐α lines we have calculated line profiles and total intensities across the Jovian disk and on the limb. For the above D columns and a H column ∼3.5×1017 cm−2, compatible with equatorial Lyman‐α airglow observations, the disk D intensity varies from 80 to 600 R for overhead Sun and viewing, whereas on the terminator the D maximum total intensity is ∼60 R at ∼860 km above the 1 bar level for the maximum D column.</div></front></TEI><affiliations><list><country><li>Canada</li><li>France</li><li>États-Unis</li></country><region><li>Michigan</li><li>Texas</li></region></list><tree><country name="Canada"><noRegion><name sortKey="Parkinson, C D" sort="Parkinson, C D" uniqKey="Parkinson C" first="C. D." last="Parkinson">C. D. Parkinson</name></noRegion><name sortKey="Griffioen, E" sort="Griffioen, E" uniqKey="Griffioen E" first="E." last="Griffioen">E. Griffioen</name><name sortKey="Mcconnell, J C" sort="Mcconnell, J C" uniqKey="Mcconnell J" first="J. C." last="Mcconnell">J. C. 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