Ogo 4 spectrometer measurements of the tropical ultraviolet airglow

Barth, C. A.; Schaffner, Sandra

doi:10.1029/ja075i022p04299

Cited by 86 publications

(26 citation statements)

References 8 publications

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“…The OI 135.6 nm emission from the low latitude ionosphere was first observed by the OGO-4 satellite, and it was observed that the low-latitude ionosphere had two emission peaks located 10°-20°from the geomagnetic equator corresponding to peaks of the plasma density of the equatorial anomaly (EA) or a.k.a. Appleton anomaly (Hicks and Chubb 1970;Barth and Schaffner 1970). Huba et al (2002) reported that the O + density deduced from the OI 135.6 nm limb scan data agrees well with the SAMI2 ionosphere model.…”

Section: Nighttime Ionospheresupporting

confidence: 68%

The Far Ultra-Violet Imager on the Icon Mission

et al. 2017

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ICON Far UltraViolet (FUV) imager contributes to the ICON science objectives by providing remote sensing measurements of the daytime and nighttime atmosphere/ionosphere. During sunlit atmospheric conditions, ICON FUV images the limb altitude profile in the shortwave (SW) band at 135.6 nm and the longwave (LW) band at 157 nm perpendicular to the satellite motion to retrieve the atmospheric O/N 2 ratio. In conditions of atmospheric darkness, ICON FUV measures the 135.6 nm recombination emission of O + ions used to compute the nighttime ionospheric altitude distribution. ICON Far UltraViolet (FUV) imager is a Czerny-Turner design Spectrographic Imager with two exit slits and corresponding back imager cameras that produce two independent images in separate wavelength bands on two detectors. All observations will be processed as limb altitude profiles. In addition, the ionospheric 135.6 nm data will be processed as longitude and latitude spatial maps to obtain images of ion distributions around regions of equatorial spread F. The ICON FUV optic axis is pointed 20 degrees below local horizontal and has a steering mirror that allows the field of view to be steered up to 30 degrees forward and aft, to keep the local magnetic meridian in the field of view. The detectors are micro channel plate (MCP) intensified FUV tubes with the phosphor fiber-optically coupled to Charge Coupled Devices (CCDs). The dual stack MCP-s amplify the photoelectron signals to overcome the CCD noise and the rapidly scanned frames are co-added to digitally create 12-second integrated images. Digital on-board signal processing is used to compensate for geometric distortion and satellite motion and to achieve data compression. The instrument was originally aligned in visible light by using a special grating and visible cameras. Final alignment, functional and environmental testing and calibration were performed in a large vacuum chamber with

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Section: Nighttime Ionospheresupporting

confidence: 68%

The Far Ultra-Violet Imager on the Icon Mission

et al. 2017

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“…Since the theoretical calculations can hardly account for such high intensities, we will examine whether a correction should be applied to the preflight calibration. The basis of the discussion is to compare intensities of the 1304-• emissions or other features observed by this instrument with the results of other measurements made under similar conditions, as was suggested initially by Barth and Schaffner [1970].…”

Section: Absolute Emission Rates Of the 1304-• Equatorial Airglowmentioning

confidence: 99%

Magnetic storm effects on the tropical ultraviolet airglow

Gérard¹,

Anderson²,

Matsushita³

1977

J. Geophys. Res.

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“…In recent years, the nature of the intertropical arcs has also been studied in the ultraviolet region (Hicks and Chubb, 1970;Barth and Schaffner, 1970), particularly the OI lines at 1304 and 1356A, and this has added a new dimension to the study of the equatorial airglow. A number of suggestions have been made for the possible origin of the ultraviolet airglow in the equatorial region, ranging from the chemical processes involving radiative recombination to the direct excitation of atomic oxygen by the precipitating energetic particles (Hanson, 1969;Hicks and Chubb, 1970;Barth and Schaffner, 1970;Knudsen, 1970;Olson, Peterson and Mosley, 1971;Zipf and Stone, 1971).…”

Section: Introductionmentioning

confidence: 99%

Equatorial airglow and the ionospheric geomagnetic anomaly

Chandra¹,

Reed²,

Troy³

et al. 1973

J. Geophys. Res.

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Ogo 4 observations of the O I (6300‐A) emissions have revealed a global pattern hitherto undetected from the ground‐based observations. It is seen that the postsunset emission of O I (6300 A) in October 1967 is very asymmetrical with respect to the geomagnetic equator in certain longitude regions and shows poor correlation with the electron density measured simultaneously from the same spacecraft. This asymmetry is less marked in the UV airglow, O I (1356 A), which appears to vary as the square of the maximum electron density in the F region. The horizon scan data of the 6300‐A airglow reveal that the latitudinal asymmetry is associated with asymmetry in the height of the O I (6300‐A) emission and hence with the altitude of the F2 peak. From the correlative studies of the airglow and the ionospheric measurements the mechanisms for the UV and the 6300‐A emissions are discussed in terms of the processes involving radiative and dissociative recombination. Theoretical expressions are developed relating the airglow data to the ionospheric parameters, and it is shown that the agreement between observed and calculated emission rates is well within the uncertainty of the measurements.

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Ogo 4 spectrometer measurements of the tropical ultraviolet airglow

Cited by 86 publications

References 8 publications

The Far Ultra-Violet Imager on the Icon Mission

The Far Ultra-Violet Imager on the Icon Mission

Magnetic storm effects on the tropical ultraviolet airglow

Equatorial airglow and the ionospheric geomagnetic anomaly

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