Space-based observations of O2 A (0,0) band emission near the solar terminator and their interpretation

Belyaev, A.N.; Alpatov, V. V.; Blanc, E.; Melnikov, V. E.

doi:10.1016/j.asr.2006.05.021

Cited by 7 publications

(4 citation statements)

References 25 publications

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“…Therefore, the reaction rate constants for reactions (7) and (8) the O 2 atm band emissions, a two-step Barth-type process, a three-body recombination reaction, [McDade et al, 1986;Marsh et al, 2002;Belyaev et al, 2006] is considered,…”

Section: The Chemical Reaction Set In the Plasma Chemistry Modelmentioning

confidence: 99%

The 762 nm emissions of sprites

et al. 2011

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[1] We report the 762 nm emissions in sprites recorded by the ISUAL experiment onboard the FORMOSAT-2 satellite. The 762 nm imager filter is centered at 763.3 nm with a 7 nm bandwidth at 50% transmittance. Sprite emissions in this passband include the N 2 first positive (1PN 2 ) bands, (2, 0) and (3, 1), the O 2 atmospheric (atm) band (0, 0), and the hydroxyl (4, 0) emissions. Because these mixed emissions cannot be resolved in the 762 nm narrowband filter, a zero-dimensional plasma chemistry model is used to estimate the expected relative intensities of these emission bands in sprites. The computed 1PN 2 brightness in a single streamer is 1.4 MR and 2.6 kR for the O 2 atm band emissions at frame integration times of 30 ms. In the 762 nm passband, the 1PN 2 emissions are the dominant emissions in sprites, and the ratio of 1PN 2 to O 2 atmospheric emissions is ∼500, while the hydroxyl emissions can be neglected. In this ISUAL 762 nm campaign, the brightest sprite out of the four recorded events has possible O 2 atm band emissions that lasted more than 90 ms, and its observed brightness is consistent with the model prediction. Even though the lightning 762 nm emissions are strongly absorbed by O 2 below 60 km, the ISUAL observed parent lightning emissions in this passband are still more than a factor of two brighter than those from ISUAL observed sprites. Hence for spacecraft nadir TLE detection missions, 762 nm bands may not be used as the sole signature to identify sprites, and auxiliary emission bands are needed.

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Section: The Chemical Reaction Set In the Plasma Chemistry Modelmentioning

confidence: 99%

The 762 nm emissions of sprites

et al. 2011

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“…These atoms and molecules release their excess energy that is caused by the solar radiation in the daytime. Atmospheric gravity waves in the mesosphere and the lower thermosphere are studied via the observations of airglow by ground‐based and spaceborne instruments [ Siskind and Sharp , ; Shepherd et al , ; Hays et al , ; Belyaev et al , ; Makela et al , ; Suzuki et al , ]. Variations in airglow emission are mainly caused by the variations of the number density and the temperature of atoms and molecules in the emission layer.…”

Section: Introductionmentioning

confidence: 99%

First spaceborne observation of the entire concentric airglow structure caused by tropospheric disturbance

Akiya

Saito

Sakanoi

et al. 2014

Geophysical Research Letters

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Spaceborne imagers are able to observe the airglow structures with wide field of views regardless of the tropospheric condition that limits the observational time of the ground‐based imagers. Concentric wave structures of the O2 airglow in 762 nm wavelength were observed over North America on 1 June 2013 from the International Space Station. This was the first observation in which the entire image of the structure was captured from space, and its spatial scale size was determined to be 1200 km radius without assumptions. The apparent horizontal wavelength was 80 km, and the amplitude in the intensity was approximately 20% of the background intensity. The propagation velocity of the structure was derived as 125 ± 62 m/s and atmospheric gravity waves were estimated to be generated for 3.5 ± 1.7 h. Concentric structures observed in this event were interpreted to be generated by super cells that caused a tornado in its early phase.

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“…Thus, one can investigate large and medium scale (more than ~100 km) phenomena using the limb measurement data. On the other hand, there are a few nadir measurements of airglow from space, in particular, in visible light such as short-term measurement from international space station (ISS) (10) . IMAGE/FUV provided nadir imaging data of ultraviolet airglow emission mainly in the low-latitude region (11) .…”

Section: Introductionmentioning

confidence: 99%

Imaging Observation of the Earth's Mesosphere, Thermosphere and Ionosphere by VISI of ISS-IMAP on the International Space Station

et al. 2011

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We present the scientific targets, instrumental design, principle of measurement, and development of the Visible and near-Infrared Spectral Imager (VISI) which will be launched onto International Space Station (ISS) in January 2012. VISI is equipped with fast optics including a grism, and a high-sensitivity CCD to obtain airglow emissions at wavelengths of O (630 nm), OH Meinel band (650 nm) and O 2 (0-0) atmospheric band (762 nm). VISI has two field-of-views (FOVs), 45 degrees forward and 45 degrees backward to nadir, to subtract background contaminations. The data acquisition of VISI will be continuously performed with short exposure cycle less than several seconds when ISS is orbiting in the night side of the earth, and then provide the seamless line scanning images of the airglows with a spatial resolution better than 50 km. After manufacturing VISI, we checked its performance though optical and electric function tests as well as environmental tests that are necessary to be launched.

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Space-based observations of O2 A (0,0) band emission near the solar terminator and their interpretation

Cited by 7 publications

References 25 publications

The 762 nm emissions of sprites

The 762 nm emissions of sprites

First spaceborne observation of the entire concentric airglow structure caused by tropospheric disturbance

Imaging Observation of the Earth's Mesosphere, Thermosphere and Ionosphere by VISI of ISS-IMAP on the International Space Station

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