Lunar tides in the mesosphere over Christmas Island (2°N, 203°E)

Stening, R. J.; Schlapp, D. M.; Vincent, R. A.

doi:10.1029/97jd00898

Cited by 20 publications

(33 citation statements)

References 18 publications

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“…Here we should note that a simple beating between the 12.42-h M 2 lunar tide and the 12 h S 2 solar tide will result in an apparent modulation of the S 2 tide at a period defined by the difference in frequency between the M 2 and S 2 tides (a frequency of ∼0.0677 cycles per day, equivalent to a period of ∼14.8 days). This latter period is close to that of the 16-day planetary wave and so may be mistakenly interpreted as resulting from a non-linear interaction between the 16-day planetary wave and the 12-h S 2 solar tide (a point noted by Stening et al, 1997b;Pancheva et al, 2002). Care must therefore be taken in attributing apparent fluctuations of the 12-h S 2 solar tide at a period near the 16 day wave to interaction with the 16-day wave.…”

Section: Discussionmentioning

confidence: 99%

“…Stening et al (1997b) compared least- squares fitting of a sum of solar and lunar tides to geophysical time series (Malin and Schlapp, 1980) in comparison to methods based on Fourier analysis (Winch and Cunningham, 1972) and concluded that the least-squares method offers a number of advantages. In particular, each hourly data point is treated separately, so scattered and/or missing data is not a problem.…”

Section: Discussionmentioning

confidence: 99%

“…In the work presented here, the analysis follows the technique of Stening et al (1997b). The time series of zonal or meridional horizontal winds, u, v(t), was taken to consist of a superposition of a number of tidal oscillations.…”

Section: Discussionmentioning

confidence: 99%

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Observations of lunar tides in the mesosphere and lower thermosphere at Arctic and middle latitudes

2006

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Abstract. Meteor radars have been used to measure the horizontal winds in the mesosphere and lower thermosphere over Castle Eaton (52 • N) in the UK and over Esrange (68 • N) in Arctic Sweden. We consider a 16-year data set covering the interval 1988-2004 for the UK and a 6-year data set covering the interval 1999-2005 for the Arctic. The signature of the 12.42-h (M 2 ) lunar tide has been identified at both locations. The lunar tide is observed to reach amplitudes as large as 11 ms −1 . The Arctic radar has an interferometer and so allows investigation of the vertical structure of the lunar tide. At both locations the tide has maximum amplitudes in winter with a second autumnal maximum. The amplitude is found to increase with height over the 80-100 km height range observed. Vertical wavelengths are very variable, ranging from about 15 km in summer to more than 60 km in winter. Comparisons with the Vial and Forbes (1994) model reveals generally good agreement, except in the case of the summer vertical wavelengths which are observed to be significantly shorter than predicted.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Observations of lunar tides in the mesosphere and lower thermosphere at Arctic and middle latitudes

2006

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“…We shall see that the phase of the eastward wind is indeed normally 90°or 3 h ahead of the northward phase but this is not always exactly so for the lunar tide. It should particularly be noted, in passing, that this phase di erence may not be 3 h for low latitude stations (Stening et al, 1997b).…”

Section: Lunar Analysismentioning

confidence: 99%

“…This model was extended to greater heights using the Global Scale Wave Model (GSWM) of Hagan et al (1995) (see Stening et al, 1997a). Results from the extended model gave fair agreement with analysed data at the near equatorial site of Christmas Island (Stening et al, 1997b). This same GSWM model is used for comparisons in this work.…”

Section: Introductionmentioning

confidence: 99%

Lunar tidal winds in the upper atmosphere over Collm

Stening

Jacobi

2000

Ann. Geophys.

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Abstract. The lunar semidiurnal tide in winds measured at around 90 km altitude has been isolated with amplitudes observed up to 4 m s )1 . There is a marked amplitude maximum in October and also a considerable phase variation with season. The average variation of phase with height indicated a vertical wavelength of more than 80 km but this, and other results, needs to be viewed in the light of the considerable averaging required to obtain statistical signi®cance. Large yearto-year variations in both amplitude and phase were also found. Some phase comparisons with the GSWM model gave reasonable agreement but the model amplitudes above a height of 100 km were much larger than those measured. An attempt to make a comparison with the lunar geomagnetic tide did not yield a statistically signi®cant result.

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Longitudinal Variation of the Lunar Tide in the Equatorial Electrojet

et al. 2017

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The atmospheric lunar tide is one known source of ionospheric variability. The subject received renewed attention as recent studies found a link between stratospheric sudden warmings and amplified lunar tidal perturbations in the equatorial ionosphere. There is increasing evidence from ground observations that the lunar tidal influence on the ionosphere depends on longitude. We use magnetic field measurements from the CHAMP satellite during July 2000 to September 2010 and from the two Swarm satellites during November 2013 to February 2017 to determine, for the first time, the complete seasonal‐longitudinal climatology of the semidiurnal lunar tidal variation in the equatorial electrojet intensity. Significant longitudinal variability is found in the amplitude of the lunar tidal variation, while the longitudinal variability in the phase is small. The amplitude peaks in the Peruvian sector (∼285°E) during the Northern Hemisphere winter and equinoxes, and in the Brazilian sector (∼325°E) during the Northern Hemisphere summer. There are also local amplitude maxima at ∼55°E and ∼120°E. The longitudinal variation is partly due to the modulation of ionospheric conductivities by the inhomogeneous geomagnetic field. Another possible cause of the longitudinal variability is neutral wind forcing by nonmigrating lunar tides. A tidal spectrum analysis of the semidiurnal lunar tidal variation in the equatorial electrojet reveals the dominance of the westward propagating mode with zonal wave number 2 (SW2), with secondary contributions by westward propagating modes with zonal wave numbers 3 (SW3) and 4 (SW4). Eastward propagating waves are largely absent from the tidal spectrum. Further study will be required for the relative importance of ionospheric conductivities and nonmigrating lunar tides.

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Lunar tides in the mesosphere over Christmas Island (2°N, 203°E)

Cited by 20 publications

References 18 publications

Observations of lunar tides in the mesosphere and lower thermosphere at Arctic and middle latitudes

Observations of lunar tides in the mesosphere and lower thermosphere at Arctic and middle latitudes

Lunar tidal winds in the upper atmosphere over Collm

Longitudinal Variation of the Lunar Tide in the Equatorial Electrojet

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