Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.11765/2224
Behavior of NO2 and O3 columns during the eclipse of February 26, 1998, as measured by visible spectroscopy
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dc.contributor.authorGil-Ojeda, Manueles_ES
dc.contributor.authorPuentedura, Olgaes_ES
dc.contributor.authorYela González, Margaritaes_ES
dc.contributor.authorCuevas Agulló, Emilioes_ES
dc.date.accessioned2016-05-03T09:15:22Z-
dc.date.available2016-05-03T09:15:22Z-
dc.date.issued2000-
dc.identifier.citationJournal of Geophysical Research: Atmospheres. 2000, 105(D3), p. 3583–3593es_ES
dc.identifier.issn2169-897X-
dc.identifier.issn2169-8996-
dc.identifier.urihttp://hdl.handle.net/20.500.11765/2224-
dc.description.abstractObservations of the NO2 and O3 columns using zenith-viewing differential absorption spectroscopy in the visible range (450–540 nm) were carried out at Izaña Observatory (Tenerife, 28°N, 16°W, 2370 m above sea level.) during the eclipse of February 26, 1998 (95% occultation over the station). Ozone has been retrieved using two different spectral ranges to minimize the effect of the continuous change of the solar spectrum shape as the Sun is being occulted. Small variations before the maximum phase in agreement with previous observations are found, but because of the change in the shape of the solar spectrum, it cannot conclusively be determined whether the ozone changes are real or due to interferences with changing Fraunhofer lines. The difficulties in observing small changes of absorbing gases during solar eclipse when using remote sensing technique that uses the solar UV and visible radiation as the source are discussed. NO2 displays an increase in phase with the degree of solar occultation, as compared to a non eclipse day of 1.55±0.09. A simple model assuming that changes over short times scales are only due to changes in photodissociation, using O3 and temperatures obtained from an ozone sounding station close to the observatory, reproduces the observed variation when the NO2 bulk is assumed to be at an altitude of 28 km. Correction for differences between local solar zenith angle (SZA) and the SZA where the absorption takes place is taken into account.es_ES
dc.description.sponsorshipThis work has been possible thanks to the support of the UE through the SCUVS-3 Project (ENV-4-CT95-0089).-
dc.formatapplication/pdf-
dc.language.isoenges_ES
dc.publisherAmerican Geophysical Uniones_ES
dc.subjectNitrogen dioxidees_ES
dc.subjectOzonees_ES
dc.subjectEclipseses_ES
dc.subjectSpectrophotometeres_ES
dc.titleBehavior of NO2 and O3 columns during the eclipse of February 26, 1998, as measured by visible spectroscopyes_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.relation.publisherversionhttps://dx.doi.org/10.1029/1999JD900973es_ES
dc.rights.accessRightsinfo:eu-repo/semantics/openAccesses_ES
Appears in Collections:Artículos científicos 2000-2004


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