Electron Excitation of the First Positive Bands of N_2 and of the First Negative and Meinel Bands of N_2^+*

Stanton, Paul; John, Robert

doi:10.1364/josa.59.000252

Cited by 112 publications

(42 citation statements)

References 11 publications

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“…. 3 in Stanton and St. John [28]. The relative fluorescence efficiency can then be normalized for each electronic state to, e. g., the most prominent band.…”

Section: Input Parametersmentioning

confidence: 99%

Impact of varying atmospheric profiles on extensive air shower observation: Fluorescence light emission and energy reconstruction

Keilhauer

Blümer

Engel³

et al. 2006

Astroparticle Physics

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Several experiments measure the fluorescence light produced by extensive air showers in the atmosphere. This light is converted into a longitudinal shower profile from which information on the primary energy and composition is derived. The fluorescence yield, as the conversion factor between light profile measured by EAS experiments and physical interpretation of showers, has been measured in several laboratory experiments. The results, however, differ considerably. In this article, a model calculation of the fluorescence emission from relevant band systems of nitrogen in dependence on wavelength and atmospheric conditions is presented. Different calculations are compared to each other in combination with varying input parameters. The predictions are compared with measurements and the altitude-dependence of the fluorescence yield is discussed in detail. PACS: 96.40.Pq

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“…. 3 in Stanton and St. John [28]. The relative fluorescence efficiency can then be normalized for each electronic state to, e. g., the most prominent band.…”

Section: Input Parametersmentioning

confidence: 99%

Impact of varying atmospheric profiles on extensive air shower observation: Fluorescence light emission and energy reconstruction

Keilhauer

Blümer

Engel³

et al. 2006

Astroparticle Physics

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“…For the excitation of atomic oxygen we have used values for the parameters of (1) suggested by R. S. Stolarski (private communication, 1972). For molecular nitrogen, molecular oxygen, and helium we have used the values given by ), and Jusick et al (1967, updated to more recent cross section measurements by Jobe et al (1967), Burns et al (1969), McConkey and, Simpson and McConkey (1969), Stanton andSt. John (1969), Brinkman andTrajmar (1970), Sheridan et al (1971), McConkey andWoolsey (1969), and Skubenich (1968).…”

Section: Cross Sectionsmentioning

confidence: 99%

Calculated photoelectron pitch angle and energy spectra

Mantas

Bowhill

1975

Planetary and Space Science

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Calculations of the steady-state photoelectron energy and angular distribution in the altitude region between 120 and 1000 km are presented.The distribution is found to be isotropic at all altitudes below 250 km, while above this altitude anisotropies in both pitch angle and energy are found. The isotropy found in the angular distribution below 250 km implies that photoelectron transport below 250 km is insignificant, while the angular anisotropy found above this altitude implies a net photoelectron current in the upward direction. The energy anisotropy above 500 km arises from the selective backscattering of the low energy photoelectron population of the upward flux component by Coulomb collisions with the ambient ions. The total photoelectron flux attains its maximum value between about 40 and 70 km above the altitude at which the photoelectron production rate is maximum. The displacement of the maximum of the equilibrium flux is attributed to an increasing (with altitude) photoelectron lifetime. Photoelectrons at altitudes above that where the flux is maximum are on the average more energetic than those below that altitude. The flux of photoelectrons escaping to the protonosphere at dawn was found to be 2.6 x 108 cm-2sec -1 , while the escaping flux at noon was found to be 1.5 x 108 cm "2 sec-1. The corresponding escaping energy fluxes are: 4.4 x 10 eV cm -2 sec -and 2.7 x 10 9 eV cm-sec -1

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“…In t e r m s of Equation (1 ) If the spectral index is independent of altitude, the ratio of the integrated column intensities w i l l also be given by Equation (4). In evaluating this ratio, we used the energy dependence of the first ositive cross section, which includes cascade from the second positive system, given by Stanton and St. John (1969) and the absolute cross section value given by Shemansky and Broadfoot (1970). The calculated ratio, 4.07, is larger than that observed on both legs of the flight, and implies that about one-half t o two-thirds of the observed 3914 A column emission is due to excitation by primary electrons.…”

Section: For Energiesmentioning

confidence: 99%

Rocket measurement of the secondary electron spectrum in an aurora

Feldman¹,

Doering²,

Moore³

1971

J. Geophys. Res.

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To be published in the Journal of The differential flux of secondary electrons with energy greater than 6 e V w a s measured in a steady I aurora with an electron spectrometer aboard an Aerobee rocket. range 10-20 eV, the observed spectrum is in excellent agreement with a recent theoretical prediction. About one-half of the observed N2+ emission at 3914 A can be accounted for by secondary electron excitation.Except for the absence of structure in the energy

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Electron Excitation of the First Positive Bands of N_2 and of the First Negative and Meinel Bands of N_2^+*

Cited by 112 publications

References 11 publications

Impact of varying atmospheric profiles on extensive air shower observation: Fluorescence light emission and energy reconstruction

Impact of varying atmospheric profiles on extensive air shower observation: Fluorescence light emission and energy reconstruction

Calculated photoelectron pitch angle and energy spectra

Rocket measurement of the secondary electron spectrum in an aurora

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