New Ultraviolet Solar Flux Measurements at 2000 Å Using a Balloon Borne Instrument

Ackerman, M.; Frimout, D.; Pastiels, R.

doi:10.1017/s0074180900103602

Cited by 6 publications

(3 citation statements)

References 2 publications

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“…Subsequent recalibration of the LASP measurements brought them closer to, but still lower than, Broadfoot's data [Mount andRottman, 1981]. Other data have been acquired from rockets[Mentall et al, 1981] and from balloons[Ackerman et al, 1971;Simon et al, 1982;Hall, 1983;Hall and Anderson, 1984]. At wavelengths between 210 and 240 nm the data from four balloon observations(in 1972, 1973, 1976, and 1977) made bySimon et al [1982] agree to within 6%.…”

mentioning

confidence: 82%

Solar ultraviolet irradiance variations: A review

Lean¹

1987

J. Geophys. Res.

280

132

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Despite the geophysical importance of solar ultraviolet radiation, specific aspects of its temporal variations have not yet been adequately determined experimentally, nor are the mechanisms for the variability completely understood. Satellite observations have verified the reality of solar ultraviolet irradiance variations over time scales of days and months, and model calculations have confirmed the association of these short‐term variations with the evolution and rotation of regions of enhanced magnetic activity on the solar disc. However, neither rocket nor satellite measurements have yet been made with sufficient accuracy and regularity to establish unequivocally the nature of the variability over the longer time of the 11‐year solar cycle. The comparative importance for the long‐term variations of local regions of enhanced magnetic activity and global scale activity perturbations is still being investigated. Solar ultraviolet irradiance variations over both short and long time scales are reviewed, with emphasis on their connection to solar magnetic activity. Correlations with ground‐based measures of solar variability are examined because of the importance of the ground‐based observations as historical proxies of ultraviolet irradiance variations. Current problems in understanding solar ultraviolet irradiance variations are discussed, and the measurements planned for solar cycle 22, which may resolve these problems, are briefly described.

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confidence: 82%

Solar ultraviolet irradiance variations: A review

Lean¹

1987

J. Geophys. Res.

280

132

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“…solar flux data ( Fig. 3) deduced by Ackerman et al (1971). Using the data tabulated by Ackerman (1971) and a ratio Arg/^a équivalent to formula (14b) (Nicolet, 1970), the results obtained are shown in Fig.…”

Section: Rg 2 Observational Data Of Solar Radiation In the 1800-225mentioning

confidence: 95%

Aeronomic chemistry of the stratosphere

Nicolet

1972

Planetary and Space Science

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In the stratosphère, dissociation of HjO, CH4 and Hu is brought about, mainly by reaction processes with excited oxygen atoms produced by the photodissociation of ozone. A discrepancy noted between theoretical and observational concentrations of O3 in the upper stratosphère suggests two possible explanations : solar radiation fluxes for O2 photodissociation which are too large along with too large rate coefficients and absorption cross sections or ozone réduction brought about by the effect of hydrogen compounds or of nitrogen oxides. The reaction of the excited oxygen atom with méthane and nitrous oxide leads to a destruction of thèse two molécules in the stratosphère which corresponds to a production of carbon monoxide with water vapor and of nitric oxide, respectively. The vertical distribution of water vapor is not affected by its dissociation in the stratosphère since ils reformation is rapid. The fact that the ratio of the hydroxyl and hydroperoxyl radical concentrations cannot be determined with adéquate précision complicates the calculation of the destruction of ozone which occurs through reactions of OH and HOj not only with atomic oxygen in the upper stratosphère but also with CO and NO in the lower stratosphère, respectively. The same difficulty arises in connection with the dissociation of nitric acid molécules formed by the reaction of OH and NOj; destruction processes by photodissociation or by reaction with OH are not yet known with précision. Another difficulty, of a différent kind, is that the nitric oxide concentration is not well known at the stratopause level.

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“…Since Callear and Pilling (1970) have revised Bethke's values of the oscillator strength for the ^(0-0) band, a correction must also be applied to the ô(l-O) band. The oscillator strength is (1-2 ± 0-2) X 10-2 and the transition probability of (5(1-0) is 2-6 X 10'' sec-^ which leads to a photodissociation coefficient at zéro optical depth /NO(^, 1-0) = (7-2 ± 1) X 10-6 sec-i 7if the radiation température is 4650° ± 50°K (Ackerman et al, 1971).…”

Section: Table 1 Electronic Oscillator Strengths Franck-condon Factmentioning

confidence: 99%

The aeronomic dissociation of nitric oxide

Cieslik

Nicolet

1973

Planetary and Space Science

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Ab stract-A detailed study is made of the atmospheric atténuation of the dissociation of nitric oxide in the mésosphère and stratosphère. The nitric oxide dissociation profile dépends on the ab sorption of the discrète Schumann-Runge b ands of Oj. The major contrib ution to the dissociation rate of NO is the predissociation of the â(O-O) and (5(1-0) b ands which can reach the stratosphère.

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New Ultraviolet Solar Flux Measurements at 2000 Å Using a Balloon Borne Instrument

Cited by 6 publications

References 2 publications

Solar ultraviolet irradiance variations: A review

Solar ultraviolet irradiance variations: A review

Aeronomic chemistry of the stratosphere

The aeronomic dissociation of nitric oxide

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