Solar wind flow past nonmagnetic planets: venus and mars.

Form of the boundary of the solar corpuscular stream produced by interaction with the magnetic dipole field of the earth

Theoretical determination of the form of the boundary of the solar corpuscular stream produced by interaction with the magnetic dipole field of the Earth

Solar plasma flow around magnetosphere, discussing plasma velocity, density and temperature and magnetic field space and time variations

Plasma flow around the magnetosphere.

Shock wave formation on interaction between solar wind & geomagnetic field - effect of weak interplanetary magnetic field

On the effect of a weak interplanetary magnetic field on the interaction between the solar wind and the geomagnetic field

The flow of the solar wind past the earth and its magnetosphere constitutes a problem similar in many ways to the familiar, but complex problem of the external aerodynamics of round-nosed bodies in a supersonic stream. It is the purpose of this paper to provide a resume of some of the basic ideas, both theoretical and experimental, that support this correspondence, and to present a connected account of many of the principal quantitative results that have been obtained through application and extension of methods developed originally for the aerodynamics of re-entry vehicles. In addition, the basic concepts of the theory of the solar wind itself are outlined in some detail in order to illustrate the basic unity of the entire theoretical description of the solar wind and its interaction with the geomagnetic field. Finally, extensive discussions of the internal consistency of the theory and the degree to which the results correspond to conditions observed in space are included for the purpose of providing an understanding of the overall reliability of the theory.

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External aerodynamics of the magnetosphere

The interaction between a neutral stream of ionized solar corpuscles and a three-dimensional magnetic dipole representing the geomagnetic fleld is investigated. It is assumed that the stream is confined to the exterior and the magnetic field to the interior of a hollow, the boundary of which is defined by a thin current sheath. An approximate method of solution is applied, and results are presented for the coordinates of the trace of the boundary of the hollow in the meridian plane containing the sun-earth line and the dipole axis for several relative orientations. Results are presented for the trace in the equatorial plane for the case in which the dipole axis is normal to the sun-earth line. The corresponding problem in two dimensions is considered, and it is shown that the analogous approximate results are in good agreement with the results indicated by an exact solution of the same basic equations. (auth)

Theoretical determination of the form of the hollow produced in the solar corpuscular stream by interaction with the magnetic dipole field of the earth

J.R. Spreiter

Papers

Theoretical determination of the form of the hollow produced in the solar corpuscular stream by interaction with the magnetic dipole field of the earth