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• W1990703619 abstract "IN recent years, plasma and magnetic field data acquired in the vicinity of the Earth, Mars, and Venus have disclosed two essentially different types of interactions with the solar wind, depending upon whether the planet has a magnetic field or not. The primary emphasis of this paper is on the application of a recently developed axisymmetric implicit unsteady Euler equation solver1'2 to the calculation of the flowfield properties of steady, axisymmetric, supersonic/hypersonic flows past blunt-nosed shapes characteristic of the interplanetary solar wind flows past both magnetic and nonmagnetic planets. The purpose is to demonstrate both the accuracy and flexibility of this new technique, as well as to present a novel application of such supersonic blunt-body procedures. Contents For a magnetic planet, a magnetosphere is established which acts as an obstacle in the supersonic flow of the solar wind. No solar wind flow crosses the boundary of the magnetosphere, termed the magnetopause, and a bow wave is established some distance upstream. For nonmagnetic planets such as Venus or Mars, the electrical conductivity and density of the upper ionosphere are sufficiently great that the solar wind is deflected around the ionosphere, with a corresponding bow wave standing off from the ionosphere boundary or ionopause. Aside from the evident differences in the underlying physical processes occurring at the two boundaries (i.e., the magnetopause and the ionopause), the principal difference between the two flows is the size of the cavity formed in the solar wind. The ionopause is wrapped much closer around Venus or Mars than the magnetopause is around Earth, the nose being at an altitude of about 500 km for Venus and probably about 175 km for Mars, compared with about 60,000 km for Earth. However, as far as the gasdynamic flow is concerned, the basic patterns are similar, with the only significant difference being the particular boundary shapes. Although somewhat surprising at first, it has been amply demonstrated3'4 that the magnetohydrodynamic equations governing solar wind flows simplify in such a fashion that the average bulk properties of the flow can be" @default.
• W1990703619 created "2016-06-24" @default.
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• W1990703619 date "1978-07-01" @default.
• W1990703619 modified "2023-10-17" @default.
• W1990703619 title "Axisymmetric Implicit Blunt-Body Computation of Solar Wind Flows Past Planets" @default.
• W1990703619 cites W1981851720 @default.
• W1990703619 cites W2025989848 @default.
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• W1990703619 doi "https://doi.org/10.2514/3.60952" @default.
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