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Auroras and Associated Phenomena

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Solar-Terrestrial Physics/1970

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 29))

Abstract

The dynamics of the auroral oval and its dependence on DP intensity are examined. Even during extremely magneto-quiet periods, auroras are observed and located along a contracted oval. In the noon sector, auroras occur at ϕ ≈ 80°, in the midnight sector at ϕ ≈ 70°. This is in agreement with observations made from satellites and aircraft.

It is shown that in the night sector the equatorward boundary of the auroral oval coincides with the projection on the polar ionosphere, along field lines, of the inner boundary of the plasma sheet in the tail. In the day sector, the equatorward boundary of the auroral oval coincides with the ‘feet’ of the outermost closed field lines. Thus, the equatorward boundary of the oval coincides with the boundary between the quasi-dipole field lines and the stretched field lines.

This relationship is then used to infer the geocentric distance of the subsolar point of the magnetopause and also the relationship between variations of the solar wind pressure and of DP intensity.

Akasofu’s pattern of the development of the auroral substorm is extended to include a new phase, called the ‘creation phase’, which is characterized by an equatorward motion of auroras in the oval in the midnight sector.

The velocity of some auroral forms during different phases of the auroral substorm is used to determine the direction and intensity of electric fields in the magnetosphere.

The amount of energy released in auroras during substorms is estimated, and its dependence on DP intensity is given.

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  1. IZMIRAN, Akademgorodok, Moscow, Russia

    Y. I. Feldstein

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E. R. Dyer

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Feldstein, Y.I. (1972). Auroras and Associated Phenomena. In: Dyer, E.R. (eds) Solar-Terrestrial Physics/1970. Astrophysics and Space Science Library, vol 29. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3693-5_26

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