Wave characteristics obtained from OH rotational temperatures and 557.7 nm airglow intensities

Cogger, L. L.; Elphinstone, R. D.; Giers, D.H.

doi:10.1016/0021-9169(88)90082-7

Cited by 9 publications

(7 citation statements)

References 20 publications

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“…Lomb-Scargle analysis of the entire database suggests the dominance of a wave of period 2.5 h and 2.6 h in OH temperature and OI 557.7 nm intensity dataset, respectively. Similar observations have been reported by Cogger et al (1988). The authors found in most cases similar wave structures in green line intensity and OH temperature.…”

Section: Gravity Wave Induced Short Period Oscillationssupporting

confidence: 90%

Observations of OI 557.7 nm nightglow at Kolhapur (17° N), India

Parihar¹,

Gurubaran

Mukherjee

2011

Ann. Geophys.

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The nocturnal behaviour of OI 557.7 nm intensity and a comparative study with simultaneous OH Meinel band temperature measurements has been presented. OI 557.7 nm intensity and OH temperature variations covary on many occasions. It was found that an 8 h tide characterizes the variation of intensity and temperature on most nights, and especially during the month of January. This is the first report of prolonged measurements of OI 557.7 nm emission from India.

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Section: Gravity Wave Induced Short Period Oscillationssupporting

confidence: 90%

Observations of OI 557.7 nm nightglow at Kolhapur (17° N), India

Parihar¹,

Gurubaran

Mukherjee

2011

Ann. Geophys.

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“…The understanding of AGW characteristics, propagation methods, and source mechanisms is important in the interpretation of the large-scale chemical and dynamic balances in this atmospheric region. Observations of airglow signatures of AGW character at the altitudes of O recombination near 95 km have been reported by Noxon [1978], Freund and Jacka [1979], Takahashi et al [1985], Taylor et al [1987], Cogger et al [1988], Swenson et al [1989], and Viereck and Deehr [1989].…”

Section: Introductionmentioning

confidence: 68%

Fabry‐Perot imaging observations of OH(8‐3): Rotational temperatures and gravity waves

Swenson¹,

Mende²,

Geller³

1990

J. Geophys. Res.

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Ground‐based observations of lower thermospheric emission originating from OH(8‐3) rotation lines P1,2 at 7316.4 Å and P2,3 at 7330 Å were made with an intensified imaging Fabry‐Perot interferometer from Santa Cruz, California, on September 25 and 26, 1987, during a CEDAR campaign. The rotational lines were imaged simultaneously from four different atmospheric volume elements which were separated by ∼15 km north to south and ∼30 km east to west. Two types of analysis are performed on the data. First, traditionally observed temporal structure in the rotational temperature showed acoustic gravity wave‐like periods which are compared to other experimental data. Spectral analysis on the data shows the traditional gravity wave characteristics for specific periods in four separated atmospheric volumes which were sampled simultaneously. Second, the simultaneous multiple‐point sample provides a measurement of horizontal phase velocity. Spectral components of temperature variation exhibited phase coherence in all four spatial regions, indicating wave phenomena of length scales ≫30 km. Gravity wave η versus period data are compared with the theories of Schubert and Walterscheid (1988) and Hickey (1988a, b).

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“…Rejection of all aurorally contaminated spectra, as has been done by others (e.g. Myrabo et al, 1987;Cogger et al, 1988), is not desirable, and thus a study of auroral detail is necessary. Table 1 gives wavelengths and K-doubling for the major P 1 lines in the OH(6±2) spectra and nearby minor features, calculated from term energies given by Coxon (1980) and Coxon and Foster (1982).…”

Section: Identi®cation Of Weak Spectral Featuresmentioning

confidence: 99%

OH(6-2) spectra and rotational temperature measurements at Davis, Antarctica

et al. 1998

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Abstract. The OH(6±2) band was monitored during 1990 at Davis, Antarctica 68X6 S, 78.0 E using a CzernyTurner scanning spectrometer. Spectra obtained with a 0.15-nm bandwidth and wavelength steps of 0.005 nm have been recorded in an attempt to isolate auroral features. This has enabled detailed study of weak features in the region k837X5À 855X5 nm. These weak features can contribute to the apparent intensity of Pbranch lines and to the background. Their presence is allowed for in our calculation of rotational temperature, but the P 1 3 line is excluded because of signi®cant contamination. An average temperature of 221 AE 2 K is obtained from a selected data set of 104 spectra. The mid-winter average temperature, for the months of May, June and July, is 224 AE 2 K, which is consistent with the 1986 CIRA model values for mid-winter at this height and latitude, but this result is dependent on the choice of transition probabilities. Preliminary assessments of seasonal and diurnal variations in rotational temperature and intensity are presented.

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Wave characteristics obtained from OH rotational temperatures and 557.7 nm airglow intensities

Cited by 9 publications

References 20 publications

Observations of OI 557.7 nm nightglow at Kolhapur (17° N), India

Observations of OI 557.7 nm nightglow at Kolhapur (17° N), India

Fabry‐Perot imaging observations of OH(8‐3): Rotational temperatures and gravity waves

OH(6-2) spectra and rotational temperature measurements at Davis, Antarctica

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