Satellite observations of OII (7320–7330 Å) emission in aurora

Cogger, L. L.; Shepherd, G. G.; Gogoshev, M. M.; Dachev, Ts.; Gerdjikova, Mariann G.

doi:10.1016/0032-0633(87)90062-6

Cited by 6 publications

(7 citation statements)

References 14 publications

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“…Torr et al (1990a), Fennelly et al (1991, Rusch et al (1977), Meriwether et al (1978) have also suggested that this emission could be a potential source to infer atomic oxygen densities. The auroral feature of this emission was reported by satellite-based observation by Cogger et al (1987). The O + ( 2 P) undergoes quenching by reacting with different constituents of the atmosphere.…”

Section: Introductionmentioning

confidence: 99%

“…It has been suggested by Cogger et al (1987), McDade et al (1991), Chang et al (1993) and Rusch et al (1977) that depending on the solar zenith angle, the secondary source contributes only 15-20% to the total production of O + ( 2 P). Further, at higher altitudes (above 250 km), there may be a possible source of O + ( 2 P) due to the photoelectron impact on O + ( 4 S).…”

Section: Modelmentioning

confidence: 99%

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Effect of solar activity on the morphology of 7320 Å dayglow emission

Krishna

Singh

2009

Ann. Geophys.

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Abstract.A comprehensive model is developed to study the 7320Å dayglow emission. The emission profiles are obtained with the help of the recently developed Solar2000 EUV (Extreme Ultra Violet) flux model. These emission profiles are used to construct the morphology of this emission between equator and 45 • N in the Northern Hemisphere. A span of five years (2001)(2002)(2003)(2004)(2005) is chosen to study the effect of solar activity on the morphology of this emission. The morphology is studied on 3 April which lies under the equinox conditions. In 2001, the solar F10.7 index on the chosen date was as high as 223.1 which is the case of solar maximum. It is found that the intensity of this emission does not vary linearly with the F10.7 solar index. The morphology shows that the region of maximum emission expands towards the higher latitudes as the F10.7 index increases.

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Section: Introductionmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

Effect of solar activity on the morphology of 7320 Å dayglow emission

Krishna

Singh

2009

Ann. Geophys.

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“…The strong correlation provides convincing evidence that O must be common variable underlying these two ratios. Cogger et al [1987] showed these data only for orbits 203 and 2377 and on that basis drew the linear fit shown. As shown in Figure 5b, the variation of 1(5577)/1(4278) is not linear, and it would be more as indicated by the dashed curve which we have added to Figure 6.…”

Section: • Emission Data There Is Little Doubt That This Emission Imentioning

confidence: 99%

Evaluation of auroral 5577‐Å excitation processes using Intercosmos Bulgaria 1300 satellite measurements

Gerdjikova¹,

Shepherd²

1987

J. Geophys. Res.

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Energy transfer from N2(A³Σu+) to O has been extensively studied as a mechanism for the production of 5577‐Å emission in the aurora, but it has yet to be fully accepted as the dominant process. This reluctance arises from the three requirements that must be met. First, the correct absolute emission rate must be produced by this mechanism. Second, the lifetime of N2(A) at auroral altitudes must be compatible with the observed time delays between the N2+ and 5577‐Å emissions. Finally, the generally accepted high degree of covariance between the N2+ and 5577‐Å emissions must be explained. This last aspect is the subject of this paper, in which we investigate this covariance in terms of spectral ratios. Measurements made from the Intercosmos Bulgaria 1300 satellite include the emission rate of the O I 5577‐Å and N2+ 4278‐Å emissions, and the flux of precipitating auroral electrons in the energy range 200 eV to 15 keV. Using the measured fluxes and atmospheric composition models, the emission rate ratio I(5577)/I(4278) for the N2(A) energy transfer mechanism is calculated and compared with the observed values. The observed ratios vary mostly from 2 to 5, with a few values outside this range. We show that this variation arises from variations in the atomic oxygen concentration, partly as an altitude effect associated with changes in primary electron energy, but more dominantly as day‐to‐day variations that are larger than those indicated by the mass spectrometer/incoherent scatter 1983 (MSIS‐83) model. Independent evidence that atomic oxygen is the source of the ratio variations is provided by correlated variations in the I(7320)/I(4278) ratio. The aspects of absolute emission rate and time delay are also reviewed, and it is concluded that the evidence is conclusively in favor of N2(A) energy transfer as the dominant auroral mechanism.

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“…It is recognized that there can also be excitation by photoelectrons from the ground‐state atomic oxygen, and while the contribution is expected to be only 10–15% [ McDade et al , ], this has not been verified by direct measurement. Excitation by electron impact is demonstrated by the appearance of the emission in the aurora [ Cogger et al , ; Semeter , ]…”

Section: Introductionmentioning

confidence: 99%

“…It is recognized that there can also be excitation by photoelectrons from the ground-state atomic oxygen, and while the contribution is expected to be only 10- been verified by direct measurement. Excitation by electron impact is demonstrated by the appearance of the emission in the aurora [Cogger et al, 1987;Semeter, 2003] The Wind Imaging Interferometer (WINDII), operated on the Upper Atmosphere Research Satellite from 1991 to 2003, has been described by Shepherd et al [1993] with a 20 year perspective on the results published recently [Shepherd et al, 2012]. For the purposes of the present study, the instrument can be treated as a simple imager with a narrowband interference filter.…”

Section: Introductionmentioning

confidence: 99%

Characteristics of the O⁺(²P–²D) 732.0 and 733.0 nm airglow emissions observed with WINDII and simulated with the C‐IAM

Shepherd

Cho

Fomichev

et al. 2014

Geophysical Research Letters

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Satellite observations of OII (7320–7330 Å) emission in aurora

Cited by 6 publications

References 14 publications

Effect of solar activity on the morphology of 7320 Å dayglow emission

Effect of solar activity on the morphology of 7320 Å dayglow emission

Evaluation of auroral 5577‐Å excitation processes using Intercosmos Bulgaria 1300 satellite measurements

Characteristics of the O⁺(²P–²D) 732.0 and 733.0 nm airglow emissions observed with WINDII and simulated with the C‐IAM

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Satellite observations of OII (7320–7330 Å) emission in aurora

Cited by 6 publications

References 14 publications

Effect of solar activity on the morphology of 7320 Å dayglow emission

Effect of solar activity on the morphology of 7320 Å dayglow emission

Evaluation of auroral 5577‐Å excitation processes using Intercosmos Bulgaria 1300 satellite measurements

Characteristics of the O+(2P–2D) 732.0 and 733.0 nm airglow emissions observed with WINDII and simulated with the C‐IAM

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Characteristics of the O⁺(²P–²D) 732.0 and 733.0 nm airglow emissions observed with WINDII and simulated with the C‐IAM