Studying the lunar tidal variations in the<i>D</i>region of the ionosphere by means of very-low-frequency phase observations

Brady, A H; Crombie, D. D.

doi:10.1029/jz068i019p05437

Cited by 14 publications

(7 citation statements)

References 5 publications

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“…(Figure 4). Thus the most significant component found by Brady and Crombie [1963] tends to support the results found here for daytime data. According to Geller [1970], the mesospheric barrier to the vertical propagation of lunar tidal energy has a minimum in winter months.…”

Section: R+ T•/• '-1 < R* < R+ T•_•/• L •supporting

confidence: 88%

“…Theory [Wait, 1964] and observation [Bickel et al, 1970] imply that VLF modes propagating between the earth and ionosphere are reflected from regions near 70 km during the day and 85.5 km during the night. Using VLF mode t'heory, Wait [1959] for the most significant daytime amplitude agree with components deduced for daytime data for a similar VLF path [Brady and Crombie, 1963]. A more extensive analysis of the effects of residual trends on the seasonally dependent results was considered unwarranted because the sample size was too small.…”

Section: R+ T•/• '-1 < R* < R+ T•_•/• L •mentioning

confidence: 97%

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DRegion lunar variations deduced from long-path 10.2-kilohertz phase measurements

Noonkester¹

1972

J. Geophys. Res.

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The relative phase of the 10.2‐kHz Omega signals propagating between Forestport, New York, and Trinidad was used to deduce semilunar components at 0400 and 1600 GMT for six 2‐month periods. The data extended from March 1, 1966, through September 1970. The average of the data phased according to the upper or lower lunar transit was subjected to harmonic analysis for a 15‐day period before and after the linear trend was removed from the average. The 15‐day periods at 0400 GMT during December and January and at 1600 GMT during February and March were significant at the 5% level. The phase of the 15‐day period changed regularly with season at 0400 and 1600 GMT, although not all seasonal components were significant. From VLF mode theory and observations the average amplitude of the 15‐day period was estimated to be 0.24 km at 85.5 km elevation (0400 GMT) and 0.06 km at 70 km elevation (1600 GMT).

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Section: R+ T•/• '-1 < R* < R+ T•_•/• L •supporting

confidence: 88%

Section: R+ T•/• '-1 < R* < R+ T•_•/• L •mentioning

confidence: 97%

DRegion lunar variations deduced from long-path 10.2-kilohertz phase measurements

Noonkester¹

1972

J. Geophys. Res.

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“…The Fourier transform spectrum of each individual series also showed the L2 line. Figure 5 As discussed in the introduction, the lunar-induced variation in VLF phase has been previously observed by Brady and Crombie [1963]. They concluded that the D region reaches a peak altitude 0.12 km above its average altitude at a lunear hour of 11.33 local lunar time.…”

Section: Lunar-induced Variationssupporting

confidence: 53%

Periodic fluctuations in the Earth‐ionosphere waveguide

Bernhardt¹,

Price²,

Crary³

1981

J. Geophys. Res.

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VLF phase and amplitude measurements made in 1967 at Byrd Station, Antarctica, using 18.6‐kHz transmissions from NLK, Washington, have been analyzed for lunar‐induced and hebdomadal variations. The VLF propagation path was 14,250 km in length and nearly constant in longitude. The lunar‐induced variations are found to be ±18° in phase and ±0.26 dB in amplitude and are explained by height changes in the D region of the ionosphere. The hebdomadal variation in VLF amplitude shows a 0.46‐dB increase during the Sunday daylight hours, relative to the Monday‐Saturday average, and is ascribed to man‐made changes in the D region.

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“…A lunar tide has been measured in the phase of the 18 kHz transmission between Panama and Boulder (Brady & Crombie 1963). This signal is certainly reflected in the D-region and the result may only be explained by assuming some lunar influence on the D-region ionization.…”

Section: L F M E a S U R E M E N T Smentioning

confidence: 99%

On the location of the ionospheric current systems responsible for the lunar and solar magnetic variations

Butcher

1980

Geophys J Int

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From a study of the sunspot cycle influence on the lunar ( L ) and solar (S) daily geomagnetic variations, Malin, Cecere & Palumbo have suggested that the electric currents responsible for these variations do not flow in the E-region as has hitherto been accepted. Indeed they suggested that the L current may even flow in the F2 region. The consequences of such a suggestion are considered and it is shown that an L current in the F-region is highly unlikely from the dynamical point of view. The evidence for Eregion currents is presented and it is suggested that the variation of E-region electron density used by Malin et al. to indicate conductivity changes in that region may not be a reliable indicator of such changes.

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Studying the lunar tidal variations in theDregion of the ionosphere by means of very-low-frequency phase observations

Cited by 14 publications

References 5 publications

DRegion lunar variations deduced from long-path 10.2-kilohertz phase measurements

DRegion lunar variations deduced from long-path 10.2-kilohertz phase measurements

Periodic fluctuations in the Earth‐ionosphere waveguide

On the location of the ionospheric current systems responsible for the lunar and solar magnetic variations

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