The Ionosphere, Sunspots, and Magnetic Storms

Kirby, S.S.; Gilliland, T.R.; Judson, E.B.; Smith, N.

doi:10.1103/physrev.48.849

Cited by 29 publications

(7 citation statements)

References 2 publications

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“…Nevertheless, the 'thermal expansion theory' remained quite popular among the ionospheric physicists of that time because it seemed to offer a plausible explanation for negative ionospheric storms (e.g. Appleton and Ingram 1935;Kirby et al 1935).…”

Section: Brief History Of Upper Atmospheric Storm Researchmentioning

confidence: 99%

Density Perturbations in the Upper Atmosphere Caused by the Dissipation of Solar Wind Energy

2010

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The upper atmosphere constitutes the outer region of the terrestrial gas envelope above about 100 km altitude. The energy budget of this outer gas layer is partly controlled by the dissipation of solar wind energy. Since this energy input is largely irregular, the resulting density changes are considered as perturbations. The properties and physics of such density perturbations are reviewed here. Besides being an important link in the complex chain of solar-terrestrial relations, such disturbances are also of practical interest because they affect the orbits of satellites and space stations and are responsible for ionospheric disturbance effects.Keywords Thermosphere (density and composition) Á Thermosphere (disturbances and storms) Á Solar-terrestrial relations (space weather effects)

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Section: Brief History Of Upper Atmospheric Storm Researchmentioning

confidence: 99%

Density Perturbations in the Upper Atmosphere Caused by the Dissipation of Solar Wind Energy

2010

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“…In spite of this work the mechanism causing ionospheric disturbances could not be clearly identified, partly because too little was known about the behavior of the neutral upper atmosphere. Early studies of auroral phenomena and also of ionospheric perturbations suggested that the neutral atmosphere might be heated during magnetic storms [e.g., Petersen, 1927;Appleton and Ingram, 1935;Kirby et al, 1935;Chapman, 1937]. However, direct evidence that this is indeed the case was only obtained many years later when Jacchia [1959] detected magnetic storm associated changes in the decay rate of artificial satellites.…”

Section: Introductionmentioning

confidence: 99%

Magnetic storm associated perturbations of the upper atmosphere: Recent results obtained by satellite‐borne gas analyzers

Prölss¹

1980

Reviews of Geophysics

313

259

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This review summarizes some of the recent results on the disturbed upper atmosphere obtained by satellite‐borne gas analyzers. According to these measurements, magnetospheric activity leads to the development of two different disturbance zones. The high‐ and middle‐latitude region is characterized by an increase in the heavier constituents Ar, N2, and O2, by a height‐dependent behavior of O, and by a significant decrease of He. The reaction time of the atmosphere is much smaller than one orbital period. At lower latitudes a moderate increase of all constituents is observed. A comparison between atmospheric and ionospheric data demonstrates that, in contrast to positive effects, negative ionospheric storms are closely coupled to changes in the neutral composition. In addition, model calculations fully support a causal relation between both phenomena. Given this correlation, atmospheric and negative ionospheric disturbance effects have certain variations in common. These include systematic changes with the magnetic storm intensity, with magnetic position, with local time, and with season. Whereas the presently available empirical and theoretical models are quite capable of reproducing the basic properties of the observed atmospheric perturbations, these algorithms are not sophisticated enough for a more detailed description of the data.

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“…Disturbances in the ionosphere associated with magnetic storms were observed in early work by Hafstad and Tuve (1929), Appleton and Ingrain (1935), Appleton et al (1937), Kirby et al (1935Kirby et al ( , 1936Kirby et al ( , 1937 and Berkner et al (1939Berkner et al ( , 1940a. The main phenomena in ionospheric F-region disturbances studied by these authors are as follows.…”

Section: Results From Earlier Workmentioning

confidence: 88%

“…However, Berkner et al (1939Berkner et al ( , 1940a found sharp and drastic depressions of NmF2 at the equatorial station Huancayo, as well as at Watheroo, within an hour after sudden commencements of severe magnetic storms. Kirby et al (1936Kirby et al ( , 1937 and Berkner et al (1939) noted increased separation between the F1 and F2 layers associated with a depression in NmF2. Kirby et al (1936Kirby et al ( , 1937 and Berkner et al (1939) noted increased separation between the F1 and F2 layers associated with a depression in NmF2.…”

Section: Results From Earlier Workmentioning

confidence: 98%

“…Principal changes in the F-region during magnetic storms are increases of the virtual height of the F2 layer, h'F2, and decreases in NmF2. An extreme case of the separation where the critical frequency of the F2 layer, foF2, becomes less than the critical frequency of the F1 layer, foF1, or so called G-condition, was found by Kirby et al (1936). An extreme case of the separation where the critical frequency of the F2 layer, foF2, becomes less than the critical frequency of the F1 layer, foF1, or so called G-condition, was found by Kirby et al (1936).…”

Section: Results From Earlier Workmentioning

confidence: 99%

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