Simulation of geophysical phenomena in the laboratory

Bachynski, M. P.

doi:10.2514/3.2706

Cited by 8 publications

(1 citation statement)

References 66 publications

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“…The major considerations of the scaling requirements pertaining to a model experiment on the interaction between the solar wind and the magnetosphere have been considered previously [Shkarofsky, 1962[Shkarofsky, , 1965Bachynski, 1964]. It seems worthwhile, however, to treat in detail the relative magnitudes of some of the parameters involved as well as several other key aspects.…”

Section: Considerations Of Some Relevant Parametersmentioning

confidence: 99%

Time History of the Magnetospheric Cavity

Osborne¹,

Bachynski²,

Gore³

1966

Radio Science

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Section: Considerations Of Some Relevant Parametersmentioning

confidence: 99%

Time History of the Magnetospheric Cavity

Osborne¹,

Bachynski²,

Gore³

1966

Radio Science

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Magnetic diffusion and the scaling laws for solar wind simulation

Riepe¹,

Young²,

Hughes

1970

Journal of Applied Mathematics and Physics (ZAMP)

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Laboratory experiments related to the solar wind and the magnetosphere

Schindler¹

1969

Reviews of Geophysics

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The increasing number of laboratory experiments related to the solar wind and the magnetosphere calls for a critical review of the conditions under which a laboratory experiment can provide information about space phenomena. Naturally, the starting point is a discussion of the problem of physical similarity. For a unified presentation of the several sets of scaling laws that have been used, it is convenient to use the similarity laws of the Vlasov theory as a reference system. Clearly, the biggest obstacle for a strict reproduction of the solar‐wind‐magnetosphere interaction in the laboratory is collisional interaction. In the solar wind at the earth's orbit, strict simulation is possible only for phenomena with a dimension of the order of a few hundred kilometers or smaller, such as the bow shock structure. A discussion of the existing terrella experiments shows that most of them obtain similarity by scaling the interplanetary field and the geomagnetic field differently. This determines the processes for which quantitative agreement can be expected, e.g., the shape of the frontal part of the cavity boundary and the approximate shape and position of the bow shock. Strict similarity can be achieved in simulating the structure of the bow shock wave. The over‐all ranges of the shock parameters of seven collision‐free shock experiments discussed cover substantial parts of the bow shock parameter ranges. A comparative discussion of the magnetic‐field profiles of the estimated shock width and of the appearance of oscillatory structures shows strong resemblances between space and laboratory observations. Several other experiments related to the solar wind and the magnetosphere are also listed.

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Simulation of geophysical phenomena in the laboratory

Cited by 8 publications

References 66 publications

Time History of the Magnetospheric Cavity

Time History of the Magnetospheric Cavity

Magnetic diffusion and the scaling laws for solar wind simulation

Laboratory experiments related to the solar wind and the magnetosphere

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