Time History of the Magnetospheric Cavity

Osborne, F. J. F.; Bachynski, M. P.; Gore, J. V.

doi:10.1002/rds196614419

Cited by 3 publications

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References 8 publications

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“…В работе Осборна и др. 50 не содержится данных об изменении параметров плазмы при изме-нении условий работы их источника, но если учесть, что приведенные в статье данные соответствуют Re m -12 и, по-видимому, отвечают лучшим режимам инжектора, то, используя имеющиеся в литературе характери-стики коаксиального инжектора, можно утверждать, что снижение вкла-дываемой энергии в три раза может снизить магнитное число Рейнольдса до единицы. Иными словами, при энергии ~700 дж в работе 50 размер магнитосферы должен стать соизмеримым с толщиной скин-слоя.…”

Section: возможность моделирования космических явленийunclassified

Physics of interplanetary plasma and laboratory experiments

Подгорный¹,

Sagdeev²

1969

Usp. Fiz. Nauk

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Section: возможность моделирования космических явленийunclassified

Physics of interplanetary plasma and laboratory experiments

Подгорный¹,

Sagdeev²

1969

Usp. Fiz. Nauk

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Hydrographische Bibliographie

Model¹,

Mädler²

1967

Deutsche Hydrographische Zeitschrift

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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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Time History of the Magnetospheric Cavity

Abstract: CFSTl PRICE(S)The visual asymmetries indicate t h a t the plasma i n the t a i l of

Cited by 3 publications

References 8 publications

Physics of interplanetary plasma and laboratory experiments

Physics of interplanetary plasma and laboratory experiments

Hydrographische Bibliographie

Laboratory experiments related to the solar wind and the magnetosphere

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