Atmospheric quantal emissions: A review of recent results

Jones, A. Vallance; Meier, R. R.; Shefov, N. N.

doi:10.1016/0021-9169(85)90099-6

Cited by 16 publications

(2 citation statements)

References 261 publications

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“…Emission lines from molecular rotationvibration bands (O 2 , N 2 , H 2 , OH, and NO 2 ) are labeled, as are some atomic transmission lines (O and Hg). Identification of emission features in this range of the spectrum is not complete (see Schmidtke et al 1985, Slanger & Huestis 1981, Jones et al 1985.…”

Section: Discussionmentioning

confidence: 99%

The First Detections of the Extragalactic Background Light at 3000, 5500, and 8000 Å. II. Measurement of Foreground Zodiacal Light

Bernstein

Freedman

Madore

2002

ApJ

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We present a measurement of the absolute surface brightness of the zodiacal light (3900-5100Å) toward a fixed extragalactic target at high ecliptic latitude based on moderate resolution (∼1.3Å per pixel) spectrophotometry obtained with the du Pont 2.5m telescope at Las Campanas Observatory in Chile. This measurement and contemporaneous Hubble Space Telescope data from WFPC2 and FOS comprise a coordinated program to measure the mean flux of the diffuse extragalactic background light (EBL). The zodiacal light at optical wavelengths results from scattering by interplanetary dust, so that the zodiacal light flux toward any extragalactic target varies seasonally with the position of the Earth. This measurement of zodiacal light is therefore relevant to the specific observations (date and target field) under discussion. To obtain this result, we have developed a technique that uses the strength of the zodiacal Fraunhofer lines to identify the absolute flux of the zodiacal light in the multiple-component night sky spectrum. Statistical uncertainties in the result are 0.6% (1σ). However, the dominant source of uncertainty is systematic errors, which we estimate to be 1.1% (1σ). We discuss the contributions included in this estimate explicitly. The systematic errors in this result contribute 25% in quadrature to the final error in our coordinated EBL measurement, which is presented in the first paper of this series.

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Section: Discussionmentioning

confidence: 99%

The First Detections of the Extragalactic Background Light at 3000, 5500, and 8000 Å. II. Measurement of Foreground Zodiacal Light

Bernstein

Freedman

Madore

2002

ApJ

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“…the photochemistry [Torr, 1985;Torr and Torr, 1982' Roble, University College London model (UCL-TGCM) of Fuller-1986a], atmospheric emissions [Bates, 1982' Rowell and Rees (1980. While these and other experimental Vallance Jones et al, 1985] and thermospheric winds and and theoretical techniques have enabled rapid progress in temperatures [e.g., Straus, 1978' Rishbeth, 1979; further quantification of the' thermosphere, it is also true Meriwether, 1983;Killeen, 1985;Rees, 1985;, that many of the basic physical processes and mechanisms Roble, 1983bRoble, ,1986b. In this contribution, I follow had already been identified and studied by prior work.…”

Section: Introductionmentioning

confidence: 99%

Energetics and dynamics of the Earth’s thermosphere

Killeen¹

1987

Reviews of Geophysics

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The Earth's thermosphere, i.e., the region above the mesopause (∼80–90 km) where the neutral gas temperature increases towards an asymptotic value determined by the variable sources of solar heating, has remained the subject of extensive experimental and theoretical study during the last few years. Since the time of the previous IUGG quadrennial report, results from several comprehensive experimental undertakings have been reported and the theoretical and semi‐empirical models of the region have matured considerably. Previous reviews in this series by Dickinson (1975), Mayr and Harris (1979), and Roble (1983a) have charted the progress made in our understanding of the thermosphere up to 1982. Other valuable review articles have appeared over the years that have concentrated on various aspects of thermospheric research including composition and variability [Carignan, 1975; Hedin, 1979; Prölss, 1980; Prölss and Roemer, 1985, 1987], incoherent scatter radar observations [Evans, 1975], tides and tidal forcing [Evans, 1978; Forbes and Garrett, 1979; Lindzen, 1979; Forbes, 1984], gravity waves [Hunsucker, 1982; Fritts 1984], ionospheric processes and electrodynamics [Richmond, 1983, 1986], thermospheric photochemistry [Torr, 1985; Torr and Torr, 1982; Roble, 1986a], atmospheric emissions [Bates, 1982, 1983; Vallance Jones et al, 1985] and thermospheric winds and temperatures [e.g., Straus, 1978; Rishbeth, 1979, 1982; Meriwether, 1983; Killeen, 1985; Rees, 1985; Mayr et al, 1985; Roble, 1983b,1986b].

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