Optical Aeronomy

Solomon, S. C.

doi:10.1002/rog.1991.29.s2.1089

Cited by 15 publications

(17 citation statements)

References 566 publications

(384 reference statements)

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“…Although the reference spectrum and scaling factors obtained from the Atmosphere Explorer (AE) program and from rocket measurements by Hinteregger et al [1981] has been considered an acceptable standard in the extreme ultraviolet (EUV) from -•30 to -•103 nm, there is considerable doubt concerning its validity shortward of -•25 nm. The problem dates back to comparisons with AE photoelectron measurements by Richards and Tort [1984], and is reviewed by Solomon [1991] and Bailey et al [2000]. Solar XUV photons are few in number, but they are energetic, variable, and important for production of photoelectrons, E-region ionization, thermospheric odd-nitrogen, and daytime airglow emissions.…”

Section: Introductionmentioning

confidence: 94%

Effect of solar soft X‐rays on the lower ionosphere

Solomon

Bailey

Woods

2001

Geophysical Research Letters

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Section: Introductionmentioning

confidence: 94%

Effect of solar soft X‐rays on the lower ionosphere

Solomon

Bailey

Woods

2001

Geophysical Research Letters

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“…The common approach [ Bates , 1992; Link and Cogger , 1988; Solomon , 1991] for the calculation of the 630.0‐ and 557.7‐nm intensities is based on the assumption that O + is the main ionospheric constituent in the nighttime F 2 region and that the O 2 + ions are only produced by the ion‐molecular reaction In this case, the O 2 + concentration can be given by the formula where n e denotes electron density and γ 2 is the rate coefficient of [ St.‐Maurice and Torr , 1978] and T eff = 0.667 T i + 0.333 T n . The values given by are in good agreement with the rate coefficients measured by Hierl et al [1997] for the nighttime temperatures.…”

Section: A Self‐consistent Airglow Model Including Molecular Ionsmentioning

confidence: 99%

“…The usual approach for the calculation of the nighttime red‐ and green‐line airglow excited in the F 2 region is based on the one‐ion approximation, [O + ] = n e , where n e denotes electron density [e.g., Bates , 1992; Link and Cogger , 1988; Solomon , 1991]. In this case, the green‐line intensity is proportional to electron density because the O( 1 S ) deactivation by collisions is negligible in the thermosphere.…”

Section: Introductionmentioning

confidence: 99%

Modeling of airglow and ionospheric parameters at Arecibo during quiet and disturbed periods in October 2002

Vlasov¹

2005

J. Geophys. Res.

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[1] The main purpose of this paper is to analyze observations of the 630.0-nm (red line) and 557.7-nm (green line) zenith airglow intensities measured during the month of October 2002 over Arecibo, Puerto Rico. We begin by describing an improved model for calculating the intensity of the red and green airglow lines that takes into account the role of molecular ions. We show, however, that at least for the data used in this study, it is not necessary to include the effects of molecular ions in our calculations. From observations of the airglow emissions on quiet days, we infer the general characteristics of the red-line intensities, which show a minimum before midnight and a peak after midnight. These results are consistent with a decrease in N m F2 and an increase in h m F2 before midnight, followed by the so-called ''midnight collapse.'' We then focus on the storm day of October 1-2, 2002, during which large-amplitude variations in both the red-and green-line intensities were observed and reproduced by the airglow model. An additional peak of N m F2, together with an h m F2 decrease, was observed before midnight, associated with the passage of a large-scale atmospheric gravity wave. The N m F2 nighttime increase requires plasma flux from the plasmasphere, which we find can be as large as 10 9 cm À2 s À1 . The plasmasphere needs an additional source of plasma in order to provide such a large flux, and we explain this by considering the role of the meridional wind in the plasma exchange process. Strong changes in the shape of the F2 region were observed during the downward and upward motion of the F2 layer during the storm period. We have found simple analytical solutions for the height distributions of the electron density in the F2 region by including the effects of recombination and diffusion. These height distributions are in excellent agreement with the measured profiles. Finally, we discuss mesospheric green-line fluctuations and show that good agreement can be obtained for the storm conditions if small adjustments are made to the eddy diffusion coefficients in the mesosphere, which we associate with the passage of the gravity wave. However, we find that some green-line behavior during quiet-time conditions is difficult to explain.

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“…Other optical emissions observed in the Earth's upper atmosphere are collectively known as airglow (and often referred to as dayglow or nightglow; Solomon, , and references therein). Airglow is the emission of light at discrete wavelengths throughout the spectrum and is produced by chemical reactions of incoming solar radiation with atoms and molecules in the upper atmosphere (Silverman, ; Solomon, ).…”

Section: Introductionmentioning

confidence: 99%

On the Origin of STEVE: Particle Precipitation or Ionospheric Skyglow?

Gallardo‐Lacourt

Liang

Nishimura

et al. 2018

Geophysical Research Letters

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One of the recent developments in ionospheric research was the introduction of a subauroral spectacle called STEVE (Strong Thermal Emission Velocity Enhancement). Although STEVE has been documented by amateur night sky watchers for decades, it is an exciting new upper atmospheric phenomenon for the scientific community. Observed first by amateur auroral photographers, STEVE appeared as a narrow luminous structure across the night sky. Currently, only one scientific study has focused on STEVE, revealing that it corresponds to a narrow (tens of kilometers in north‐south extent) and long (thousands of kilometers in east‐west direction) structure located in the subauroral region. An important and fundamental question that arises from this study is the origin of STEVE; more specifically, does STEVE correspond to a new ionospheric phenomenon or is it due to particle precipitation? In this letter, we analyze a STEVE event on 28 March 2008 observed by Time History of Events and Macroscale Interactions during Substorms (THEMIS) ground‐based All‐Sky Imagers and a Polar Orbiting Environmental Satellite (POES). The POES‐17 satellite crossed STEVE at the center of the All‐Sky Imager field‐of‐view, allowing us to collect particle data simultaneously. These concurrent measurements show that STEVE might not be associated with particle precipitation (electrons or ions). Therefore, this event suggests that STEVE's skyglow (which we defined to be unrelated to aurora or airglow) could be generated in the ionosphere.

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Optical Aeronomy

Cited by 15 publications

References 566 publications

Effect of solar soft X‐rays on the lower ionosphere

Effect of solar soft X‐rays on the lower ionosphere

Modeling of airglow and ionospheric parameters at Arecibo during quiet and disturbed periods in October 2002

On the Origin of STEVE: Particle Precipitation or Ionospheric Skyglow?

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