Night airglow intensity variations in the [O I] 5577 A, [O I] 6300 A, and NaI 5890-96 A emission lines

Smith, L. L.; Steiger, Walter R.

doi:10.1029/ja073i007p02531

Cited by 22 publications

(3 citation statements)

References 12 publications

(8 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In addition, the daily variation of this emission has also been investigated, showing the presence of a general maximum near midnight [ Dufay and Tcheng , 1946; Roach and Petit , 1951; Christophe‐Glaume , 1965; Fukuyama , 1976; Petididier , 1978]. However, this maximum was not always found by others [ Smith and Owen , 1966; Smith and Steiger , 1968]. Brenton and Silverman [1970] carefully investigated the latitudinal variation of the diurnal variation, and found it could be best described by separating the stations into three latitude bands.…”

Section: Introductionmentioning

confidence: 99%

Long‐term behavior of the OI 558 nm emission in the night sky and its aeronomical implications

Deutsch

2003

J. Geophys. Res.

View full text Add to dashboard Cite

[1] Study of the long-term behavior of the OI 558 nm emission in the night-sky, using data encompassing observations at low geomagnetic activity from 1923 to present, gives the result that these long-term, noisy, geophysical time series need to include nearly 20 cycles of an oscillation before a stable statistically meaningful answer is achieved. Periodogram analysis reveals that the strongest and predominant statistically significant oscillation in the OI 558 nm emission is a yearly variation. When this yearly oscillation is the main oscillation present in the spectrum, it has a fractional amplitude of value near 0.4. A semiannual oscillation is often also found in addition to the annual oscillation and, when significant annual and semiannual components are present, the fractional amplitudes are typically near 0.3 and 0.2 for the annual and semiannual oscillations, respectively. However, the annual fractional amplitude increases with latitude, while the semiannual fractional amplitude decreases with latitude. These results provide an insight on the nature of the seasonal variation of the OI 558 nm emission. Our longest time series are about 12 years long and thus set the lowest frequency to be studied. It is found that the OI 558 nm emission rate increases with solar activity, but in general, the emission is higher during the decreasing phase of solar activity; the apparent relationship changes with different solar cycles. OI 558 nm emission observations have been used to provide observational constraints to global dynamical atmospheric models. However, those constraining observational series have been of limited length and location and are possibly atypical. In the context of a model constrained by such observations, one can infer differences in the dynamical behavior of the atmosphere with latitude in order to account for the observed climatological emission behavior.

show abstract

Section: Introductionmentioning

confidence: 99%

Long‐term behavior of the OI 558 nm emission in the night sky and its aeronomical implications

Deutsch

2003

J. Geophys. Res.

View full text Add to dashboard Cite

show abstract

“…Also, very recently, Swider (1986a) made a connection between the known equinoctal maxima of ozone and a less well known peak in the sodium nightglow at the equinoxes [Smith and Steiger, 1968;Kirchhoff et al, 1979]. He suggested that in the chemistry of the sodium D-line nightglow the sodium remained unconsumed, and that the seasonal variations of sodium density and the nightglow were uncoupled.…”

Section: (A)mentioning

confidence: 99%

Nighttime Na D emission observed from a polar‐orbiting DMSP satellite

Newman¹

1988

J. Geophys. Res.

View full text Add to dashboard Cite

Limb scans of nighttime sodium doublet emissions at 589 nm were performed globally from a Sun‐synchronous satellite during July 1979. The observations have provided a global description of variation in the emitting layer with latitude and altitude. The limb scan data are consistent with the presence of a 10‐km‐thick emitting layer near the 90‐km peak of the sodium density in the northern mid‐latitude mesosphere in summer. At equatorial and southern latitudes, however, a narrower emission layer occurs 5–10 km lower, and the intensity is stronger by a factor of 3 or more. It appears likely that the shape of the Na D emission profile is influenced by the altitude distributions of both sodium and ozone, the reactants which are necessary to produce the emission. The observed variability may be explained by a systematic seasonal mismatch in the altitude of the mesospheric density maxima for sodium and ozone, combined with a known threefold wintertime increase in sodium density.

show abstract

“…However, investigations of daily variation of OI5577 do not show clear characteristics pertaining to maxima or minma during daily observation. Some of the studies show the presence of a general maximum near midnight (e.g., Christophe-Glaume 1965), but others do not show the same behavior (Smith and Steiger 1968). Some studies also show a correlation between geomagnetic activity and the OI5577 emission rate (e.g., Silverman 1970;Hernandez 1976); in particular, during high geomagnetic activity, measured by the Kp index, enhanced auroral activity and thermospheric temperature may contribute to the OI5577 emission rate.…”

Section: Introductionmentioning

confidence: 97%