First UV satellite observations of mesospheric water vapor
Identifieur interne : 002321 ( Main/Exploration ); précédent : 002320; suivant : 002322First UV satellite observations of mesospheric water vapor
Auteurs : Michael H. Stevens [États-Unis] ; R. L. Gattinger [Canada] ; J. Gumbel [Suède] ; E. J. Llewellyn [Canada] ; D. A. Degenstein [Canada] ; M. Khaplanov [Suède] ; G. Witt [Suède]Source :
- Journal of Geophysical Research: Atmospheres [ 0148-0227 ] ; 2008-06-27.
Abstract
We report the first UV satellite observations of mesospheric water vapor. The measurements are of nonthermal OH prompt emission between 300–330 nm produced directly from the photodissociation of water vapor by H Lyman‐α. This technique is most sensitive to water vapor concentrations between 70–90 km altitude. We present OH data from two limb scanning experiments: the Middle Atmosphere High Resolution Spectrograph Investigation (MAHRSI) and the Optical Spectrograph and Infra‐Red Imager System (OSIRIS). Interpretation of the lower resolution (∼1 nm) OSIRIS spectra requires the rotational emission rate factors for OH(1,1) solar fluorescence between 313–318 nm, which we present for the first time herein. Comparison of water vapor concentration profiles with the most coincident profiles from the Halogen Occultation Experiment on the Upper Atmosphere Research Satellite shows agreement to within 30% between 75–80 km for both MAHRSI and OSIRIS. We discuss the benefits of this promising new approach to measuring upper mesospheric water vapor and the need for new laboratory measurements to improve the analysis.
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DOI: 10.1029/2007JD009513
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The measurements are of nonthermal OH prompt emission between 300–330 nm produced directly from the photodissociation of water vapor by H Lyman‐α. This technique is most sensitive to water vapor concentrations between 70–90 km altitude. We present OH data from two limb scanning experiments: the Middle Atmosphere High Resolution Spectrograph Investigation (MAHRSI) and the Optical Spectrograph and Infra‐Red Imager System (OSIRIS). Interpretation of the lower resolution (∼1 nm) OSIRIS spectra requires the rotational emission rate factors for OH(1,1) solar fluorescence between 313–318 nm, which we present for the first time herein. Comparison of water vapor concentration profiles with the most coincident profiles from the Halogen Occultation Experiment on the Upper Atmosphere Research Satellite shows agreement to within 30% between 75–80 km for both MAHRSI and OSIRIS. We discuss the benefits of this promising new approach to measuring upper mesospheric water vapor and the need for new laboratory measurements to improve the analysis.</div></front></TEI><affiliations><list><country><li>Canada</li><li>Suède</li><li>États-Unis</li></country><region><li>Svealand</li></region><settlement><li>Stockholm</li></settlement><orgName><li>Université de Stockholm</li></orgName></list><tree><country name="États-Unis"><noRegion><name sortKey="Stevens, Michael H" sort="Stevens, Michael H" uniqKey="Stevens M" first="Michael H." last="Stevens">Michael H. Stevens</name></noRegion></country><country name="Canada"><noRegion><name sortKey="Gattinger, R L" sort="Gattinger, R L" uniqKey="Gattinger R" first="R. L." last="Gattinger">R. L. Gattinger</name></noRegion><name sortKey="Degenstein, D A" sort="Degenstein, D A" uniqKey="Degenstein D" first="D. A." last="Degenstein">D. A. Degenstein</name><name sortKey="Llewellyn, E J" sort="Llewellyn, E J" uniqKey="Llewellyn E" first="E. J." last="Llewellyn">E. J. Llewellyn</name></country><country name="Suède"><region name="Svealand"><name sortKey="Gumbel, J" sort="Gumbel, J" uniqKey="Gumbel J" first="J." last="Gumbel">J. Gumbel</name></region><name sortKey="Khaplanov, M" sort="Khaplanov, M" uniqKey="Khaplanov M" first="M." last="Khaplanov">M. Khaplanov</name><name sortKey="Witt, G" sort="Witt, G" uniqKey="Witt G" first="G." last="Witt">G. Witt</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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