The variability of 558nm OI nightglow intensity measured over Adelaide, Australia

Woithe, J. M.

doi:10.1016/j.asr.2007.01.061

Cited by 11 publications

(25 citation statements)

References 30 publications

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“…In Reid and Woithe [, hereinafter RW07] we reported on 11 years of OI nightglow intensity made using a three‐field photometer (3FP) located at the BP field site. We found the annual and semiannual oscillations to have about equal intensity, with amplitudes of between 17 (±5) % and 14 (±5) % of the mean intensity, respectively.…”

Section: Introductionmentioning

confidence: 88%

Seasonal variations of the nighttime O(¹S) and OH (8‐3) airglow intensity at Adelaide, Australia

2014

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We analyze 15 years of atomic oxygen (OI) 558 nm and hydroxyl (OH) (8-3) 730 nm nightglow emission intensities from heights near 96 and 87 km, respectively, measured using filter photometers at the Buckland Park Field Station (34.6°S, 138.6°E) near Adelaide, Australia. The intensity of both emissions exhibits clear seasonal and interannual periodicities, with annual, semiannual, and quasi-biennial oscillations, as well as a solar cycle influence. In addition, there is a terannual and 4.1 year component in the OI airglow intensity and both a quasi-biennial and quasi-triennial oscillation in the OH intensity. The results are in very good agreement with simultaneous collocated measurements made with an imager, and with global satellite climatologies of OI and OH intensities reported for the Wind Imaging Interferometer instrument. The mean value of the OI annual oscillation intensity is the same as that of the semiannual oscillation at this location to within the experimental uncertainty. The OI annual oscillation maximizes in summer, and the semiannual oscillation maximizes in autumn and spring, with the largest maximum in autumn. The terannual component in the OI nightglow maximizes in early summer, autumn, and spring. The quasi-biennial oscillation in the OI nightglow takes its first maximum value in autumn 1996, and the 4.1 year period in this emission first maximizes in summer 1998. The OH annual and semiannual oscillation intensities also agree to within the experimental uncertainties and are observed to peak in early winter. The quasi-biennial and quasi-triennial oscillations in this emission take their first maximum value in summer 1996.

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Section: Introductionmentioning

confidence: 88%

Seasonal variations of the nighttime O(¹S) and OH (8‐3) airglow intensity at Adelaide, Australia

2014

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“…Sierra Nevada data show a larger annual component than that observed at Adelaide, but the magnitude and phase of the semiannual oscillation is consistent with the observations and the TIME‐GCM model. However, O2A temperature data from Reid and Woithe [2007] presented in Table 2 suggest a weaker annual oscillation at Adelaide, accompanied by a significantly larger semiannual oscillation. The combined amplitudes indicate a slightly larger April temperature maximum, in contrast to the stronger September maximum suggested by the imager data.…”

Section: Data Presentation and Analysismentioning

confidence: 95%

A seasonal study of mesospheric temperatures and emission intensities at Adelaide and Alice Springs

et al. 2008

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[1] Aerospace imagers operating at Alice Springs (23°42 0 S, 133°530 E) and Adelaide (34°55 0 S, 138°36 0 E) have collected more than 4-year of OH and O 2 atmospheric emission data. Images taken over the course of each moonless night at 5-min intervals were used to determine OH Meinel (6, 2) and O 2 Atmospheric (0, 1) band emission intensities and temperatures, as well as atmospheric gravity wave parameters. The NCAR general circulation model TIME-GCM was run for years [2002][2003][2004][2005] for comparison with these data. The data presented here show the interannual variability of OH and O2A emissions at two sites, Alice Springs and Adelaide, over a 4-a period. It was found that the TIME-GCM successfully reproduces many observed features of the data, including equinoctial maxima associated with the diurnal tide, a 6-h phase shift between OH temperature and intensity maxima, and springtime OH intensity enhancements at Alice Springs. However, the model tends to underestimate the depth of the summertime temperature minimum at both sites, possibly due to inadequate specification of the seasonal variation of gravity waves in the model. The model does, however, successfully describe many of the mesospheric changes observed during the 2002 stratospheric warming event.

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“…There have been many ground-based and satellite-based studies in the past that addressed the short-and long-term variations of the oxygen green line emission (Brenton and Silverman, 1970;Donahue et al, 1973;Fukuyama, 1976Fukuyama, , 1977Cogger et al, 1981;Shepherd et al, 1995Shepherd et al, , 2005Yee et al, 1997;Deutsch and Hernandez, 2003;Reid and Woithe, 2007;Das and Sinha, 2008;Liu and Shepherd, 2008;Liu et al, 2008a, b).…”

Section: Introductionmentioning

confidence: 99%

“…Shiokawa and Kiyama (2000) also investigated the Kiso data (1979)(1980)(1981)(1982)(1983)(1984)(1985)(1986)(1987)(1988)(1989)(1990)(1991)(1992)(1993)(1994) and found the presence of two seasonal peaks, one in June and the other in October, however, no detailed spectral analysis was performed. Reid and Woithe (2007) used a 11 year long database of oxygen green line nightglow observations over Buckland Park (34.9…”

Section: Introductionmentioning

confidence: 99%

Effects of solar cycle variations on oxygen green line emission rate over Kiso, Japan

2011

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A sixteen year long dataset of mesospheric OI 557.7 nm green line nightglow emission rate, measured over Kiso (35.79 • N, 137.63• E), Japan using ground-based photometers is spectrally investigated using the HilbertHuang Transform (HHT). The spectrograms reveal the presence of semi-annual, annual and quasi-biennial oscillations in consonance with the results obtained from wavelet analysis in an earlier study. In addition, due to the use of the HHT, we have been able to investigate the very low frequency solar cycle variation in the emission rate. It is found that there is a signi cant solar cycle effect on the oxygen green line emission rate. The mean amplitude of variation is approximately 20% and it is also found that it is maximum at midnight. A correlation study between the means of the emission rate and the solar radio ux at 10.7 cm also shows that the effect of solar activity on the oxygen green line emission rate is maximum at midnight.

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The variability of 558nm OI nightglow intensity measured over Adelaide, Australia

Cited by 11 publications

References 30 publications

Seasonal variations of the nighttime O(¹S) and OH (8‐3) airglow intensity at Adelaide, Australia

Seasonal variations of the nighttime O(¹S) and OH (8‐3) airglow intensity at Adelaide, Australia

A seasonal study of mesospheric temperatures and emission intensities at Adelaide and Alice Springs

Effects of solar cycle variations on oxygen green line emission rate over Kiso, Japan

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The variability of 558nm OI nightglow intensity measured over Adelaide, Australia

Cited by 11 publications

References 30 publications

Seasonal variations of the nighttime O(1S) and OH (8‐3) airglow intensity at Adelaide, Australia

Seasonal variations of the nighttime O(1S) and OH (8‐3) airglow intensity at Adelaide, Australia

A seasonal study of mesospheric temperatures and emission intensities at Adelaide and Alice Springs

Effects of solar cycle variations on oxygen green line emission rate over Kiso, Japan

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Seasonal variations of the nighttime O(¹S) and OH (8‐3) airglow intensity at Adelaide, Australia

Seasonal variations of the nighttime O(¹S) and OH (8‐3) airglow intensity at Adelaide, Australia