AustralieFrV1, PascalFrancis, Checkpoint, bibRecord, 002715

Visible and near-infrared nightglow of molecular oxygen in the atmosphere of Venus

Identifieur interne : 002715 ( PascalFrancis/Checkpoint ); précédent : 002714; suivant : 002716

Visible and near-infrared nightglow of molecular oxygen in the atmosphere of Venus

Auteurs : A. Garcia Munoz [Australie, France] ; F. P. Mills [Australie] ; T. G. Slanger [États-Unis] ; G. Piccioni [Italie]

Source :

Journal of geophysical research [ 0148-0227 ] ; 2009.

RBID : Pascal:10-0100458

Descripteurs français

Pascal (Inist)
- Luminescence nocturne, Oxygène, Atmosphère, Planète Vénus, Spectre IR proche, Instrumentation, Haute atmosphère, Latitude, Altitude, Recombinaison, Dioxyde de carbone, Constante vitesse, Modèle 1 dimension, Raie verte, Gaz effet serre.
Wicri :
- topic : Oxygène, Atmosphère.

English descriptors

KwdEn :
- Carbon dioxide, Green line, Near infrared spectrum, Nightglow, Rate constant, Recombination, Upper atmosphere, Venus, altitude, atmosphere, greenhouse gas, instruments, latitude, one-dimensional models, oxygen.

Abstract

[1] The Herzberg II system of O₂ has been a known feature of Venus' nightglow since the Venera 9 and 10 orbiters detected its c(0)-X(v") progression more than 3 decades ago. We search for its emission at 400 nm-700 nm in spectra obtained with the VIRTIS instrument on Venus Express. Despite the weakness of the signal, integration over a few hours of limb observations of the planet's upper atmosphere reveals the unambiguous pattern of the progression. The selected data sample mainly the northern latitudes within a few hours of local midnight. The emission is ubiquitous on the nightside of Venus and can be discerned at tangent altitudes from 80 km to 110 km. The average emission vertical profiles of the c(0)-X(v") progression and the O₂ a(0)-X(0) band, the latter from simultaneous near-infrared spectra, are quite similar, with their respective peaks occurring within ±1 km of each other. We conclude that the net yield for production of the c(0) state is low, ∼1%-2% of the oxygen recombination rate, and that O(³P) and CO₂ are the two likely quenchers of the Herzberg II nightglow, although CO cannot be ruled out. We also derive a value of 2.45 x 10^-16 cm³ s^-1 for the rate constant at which CO₂ collisionally quenches the c(0) state. Our VIRTIS spectra show hints of O₂ A'(0)-a(v") emission but no traces of the O (¹S-¹D) green line at 557.7 nm.

Affiliations:

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Le document en format XML

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<term>Haute atmosphère</term>
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<term>Altitude</term>
<term>Recombinaison</term>
<term>Dioxyde de carbone</term>
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<term>Modèle 1 dimension</term>
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<front><div type="abstract" xml:lang="en">[1] The Herzberg II system of O<sub>2</sub>
 has been a known feature of Venus' nightglow since the Venera 9 and 10 orbiters detected its c(0)-X(v") progression more than 3 decades ago. We search for its emission at 400 nm-700 nm in spectra obtained with the VIRTIS instrument on Venus Express. Despite the weakness of the signal, integration over a few hours of limb observations of the planet's upper atmosphere reveals the unambiguous pattern of the progression. The selected data sample mainly the northern latitudes within a few hours of local midnight. The emission is ubiquitous on the nightside of Venus and can be discerned at tangent altitudes from 80 km to 110 km. The average emission vertical profiles of the c(0)-X(v") progression and the O<sub>2</sub>
 a(0)-X(0) band, the latter from simultaneous near-infrared spectra, are quite similar, with their respective peaks occurring within ±1 km of each other. We conclude that the net yield for production of the c(0) state is low, ∼1%-2% of the oxygen recombination rate, and that O(<sup>3</sup>
P) and CO<sub>2</sub>
 are the two likely quenchers of the Herzberg II nightglow, although CO cannot be ruled out. We also derive a value of 2.45 x 10<sup>-16</sup>
 cm<sup>3</sup>
 s<sup>-1</sup>
 for the rate constant at which CO<sub>2</sub>
 collisionally quenches the c(0) state. Our VIRTIS spectra show hints of O<sub>2</sub>
 A'(0)-a(v") emission but no traces of the O (<sup>1</sup>
S-<sup>1</sup>
D) green line at 557.7 nm.</div>
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<fC01 i1="01" l="ENG"><s0>[1] The Herzberg II system of O<sub>2</sub>
 has been a known feature of Venus' nightglow since the Venera 9 and 10 orbiters detected its c(0)-X(v") progression more than 3 decades ago. We search for its emission at 400 nm-700 nm in spectra obtained with the VIRTIS instrument on Venus Express. Despite the weakness of the signal, integration over a few hours of limb observations of the planet's upper atmosphere reveals the unambiguous pattern of the progression. The selected data sample mainly the northern latitudes within a few hours of local midnight. The emission is ubiquitous on the nightside of Venus and can be discerned at tangent altitudes from 80 km to 110 km. The average emission vertical profiles of the c(0)-X(v") progression and the O<sub>2</sub>
 a(0)-X(0) band, the latter from simultaneous near-infrared spectra, are quite similar, with their respective peaks occurring within ±1 km of each other. We conclude that the net yield for production of the c(0) state is low, ∼1%-2% of the oxygen recombination rate, and that O(<sup>3</sup>
P) and CO<sub>2</sub>
 are the two likely quenchers of the Herzberg II nightglow, although CO cannot be ruled out. We also derive a value of 2.45 x 10<sup>-16</sup>
 cm<sup>3</sup>
 s<sup>-1</sup>
 for the rate constant at which CO<sub>2</sub>
 collisionally quenches the c(0) state. Our VIRTIS spectra show hints of O<sub>2</sub>
 A'(0)-a(v") emission but no traces of the O (<sup>1</sup>
S-<sup>1</sup>
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<fC02 i1="01" i2="3"><s0>001E</s0>
</fC02>
<fC02 i1="02" i2="2"><s0>001E01</s0>
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<fC02 i1="03" i2="2"><s0>220</s0>
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<fC03 i1="01" i2="X" l="FRE"><s0>Luminescence nocturne</s0>
<s5>01</s5>
</fC03>
<fC03 i1="01" i2="X" l="ENG"><s0>Nightglow</s0>
<s5>01</s5>
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<fC03 i1="01" i2="X" l="SPA"><s0>Luminiscencia nocturna</s0>
<s5>01</s5>
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<s5>02</s5>
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<s5>02</s5>
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<fC03 i1="02" i2="2" l="SPA"><s0>Oxígeno</s0>
<s5>02</s5>
</fC03>
<fC03 i1="03" i2="2" l="FRE"><s0>Atmosphère</s0>
<s5>03</s5>
</fC03>
<fC03 i1="03" i2="2" l="ENG"><s0>atmosphere</s0>
<s5>03</s5>
</fC03>
<fC03 i1="03" i2="2" l="SPA"><s0>Atmósfera</s0>
<s5>03</s5>
</fC03>
<fC03 i1="04" i2="2" l="FRE"><s0>Planète Vénus</s0>
<s5>04</s5>
</fC03>
<fC03 i1="04" i2="2" l="ENG"><s0>Venus</s0>
<s5>04</s5>
</fC03>
<fC03 i1="04" i2="2" l="SPA"><s0>Planeta Venus</s0>
<s5>04</s5>
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<s5>05</s5>
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<s5>05</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Espectro IR próximo</s0>
<s5>05</s5>
</fC03>
<fC03 i1="06" i2="2" l="FRE"><s0>Instrumentation</s0>
<s5>06</s5>
</fC03>
<fC03 i1="06" i2="2" l="ENG"><s0>instruments</s0>
<s5>06</s5>
</fC03>
<fC03 i1="06" i2="2" l="SPA"><s0>Instrumentación</s0>
<s5>06</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Haute atmosphère</s0>
<s5>07</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Upper atmosphere</s0>
<s5>07</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Alta atmósfera</s0>
<s5>07</s5>
</fC03>
<fC03 i1="08" i2="2" l="FRE"><s0>Latitude</s0>
<s5>08</s5>
</fC03>
<fC03 i1="08" i2="2" l="ENG"><s0>latitude</s0>
<s5>08</s5>
</fC03>
<fC03 i1="09" i2="2" l="FRE"><s0>Altitude</s0>
<s5>09</s5>
</fC03>
<fC03 i1="09" i2="2" l="ENG"><s0>altitude</s0>
<s5>09</s5>
</fC03>
<fC03 i1="09" i2="2" l="SPA"><s0>Altitud</s0>
<s5>09</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Recombinaison</s0>
<s5>10</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Recombination</s0>
<s5>10</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Recombinación</s0>
<s5>10</s5>
</fC03>
<fC03 i1="11" i2="X" l="FRE"><s0>Dioxyde de carbone</s0>
<s2>NK</s2>
<s2>FX</s2>
<s5>11</s5>
</fC03>
<fC03 i1="11" i2="X" l="ENG"><s0>Carbon dioxide</s0>
<s2>NK</s2>
<s2>FX</s2>
<s5>11</s5>
</fC03>
<fC03 i1="11" i2="X" l="SPA"><s0>Carbono dióxido</s0>
<s2>NK</s2>
<s2>FX</s2>
<s5>11</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE"><s0>Constante vitesse</s0>
<s5>12</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG"><s0>Rate constant</s0>
<s5>12</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA"><s0>Constante velocidad</s0>
<s5>12</s5>
</fC03>
<fC03 i1="13" i2="2" l="FRE"><s0>Modèle 1 dimension</s0>
<s5>13</s5>
</fC03>
<fC03 i1="13" i2="2" l="ENG"><s0>one-dimensional models</s0>
<s5>13</s5>
</fC03>
<fC03 i1="13" i2="2" l="SPA"><s0>Modelo 1 dimensión</s0>
<s5>13</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Raie verte</s0>
<s5>14</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG"><s0>Green line</s0>
<s5>14</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA"><s0>Raya verde</s0>
<s5>14</s5>
</fC03>
<fC03 i1="15" i2="2" l="FRE"><s0>Gaz effet serre</s0>
<s5>15</s5>
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<fC03 i1="15" i2="2" l="ENG"><s0>greenhouse gas</s0>
<s5>15</s5>
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<fN21><s1>067</s1>
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<fN44 i1="01"><s1>OTO</s1>
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<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
<affiliations><list><country><li>Australie</li>
<li>France</li>
<li>Italie</li>
<li>États-Unis</li>
</country>
<region><li>Californie</li>
<li>Latium</li>
</region>
<settlement><li>Rome</li>
</settlement>
</list>
<tree><country name="Australie"><noRegion><name sortKey="Garcia Munoz, A" sort="Garcia Munoz, A" uniqKey="Garcia Munoz A" first="A." last="Garcia Munoz">A. Garcia Munoz</name>
</noRegion>
<name sortKey="Mills, F P" sort="Mills, F P" uniqKey="Mills F" first="F. P." last="Mills">F. P. Mills</name>
<name sortKey="Mills, F P" sort="Mills, F P" uniqKey="Mills F" first="F. P." last="Mills">F. P. Mills</name>
</country>
<country name="France"><noRegion><name sortKey="Garcia Munoz, A" sort="Garcia Munoz, A" uniqKey="Garcia Munoz A" first="A." last="Garcia Munoz">A. Garcia Munoz</name>
</noRegion>
</country>
<country name="États-Unis"><region name="Californie"><name sortKey="Slanger, T G" sort="Slanger, T G" uniqKey="Slanger T" first="T. G." last="Slanger">T. G. Slanger</name>
</region>
</country>
<country name="Italie"><region name="Latium"><name sortKey="Piccioni, G" sort="Piccioni, G" uniqKey="Piccioni G" first="G." last="Piccioni">G. Piccioni</name>
</region>
</country>
</tree>
</affiliations>
</record>

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{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
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   |type=    RBID
   |clé=     Pascal:10-0100458
   |texte=   Visible and near-infrared nightglow of molecular oxygen in the atmosphere of Venus
}}

This area was generated with Dilib version V0.6.33.
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	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

Visible and near-infrared nightglow of molecular oxygen in the atmosphere of Venus

Visible and near-infrared nightglow of molecular oxygen in the atmosphere of Venus

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Abstract

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