3-D computational model for solar wind/magnetosphere interactions - prediction of polar flattening of Jupiter and Saturn magnetospheres

Conference · Mon Jun 01 04:00:00 EDT 1987 · AIAA J.; (United States)

OSTI ID:6016202

Stahara, S S; Rachiele, R R; Spreiter, J R; Slavin, J A

The development of a computational model for determining the solution of the gasdynamic portion of the gasdynamic convected magnetic field model for solar wind flow past three-dimensional magnetoionopauses of nonaxisymmetric shape is described. Results are presented for the shape of the bow wave and the flow properties in magnetosheaths of polar flattened magnetopauses representative of Jupiter and Saturn. Through a parametric study in which the amount of polar flattening is varied, a quantitative determination is obtained of the degree of flattening at both Jupiter and Saturn. These new three-dimensional results are shown to be in good agreement with observations, and account for most of the differences between the observations and the axisymmetric model results. 18 references.

• Research Organization: RMA Aerospace, Inc., Mountain View, CA; Stanford Univ., CA; NASA, Washington, DC
• OSTI ID: 6016202
• Report Number(s): AIAA-Paper-87-1411; CONF-870622-
• Conference Information: Journal Name: AIAA J.; (United States)
• Country of Publication: United States
• Language: English

Related Subjects

640107* -- Astrophysics & Cosmology-- Planetary Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CONSERVATION LAWS
FLUID MECHANICS
HYDRODYNAMICS
INTERACTIONS
JUPITER PLANET
MAGNETIC FIELD CONFIGURATIONS
MAGNETOHYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
PARAMETRIC ANALYSIS
PLANETARY ATMOSPHERES
PLANETARY MAGNETOSPHERES
PLANETS
SATURN PLANET
SHOCK WAVES
SOLAR ACTIVITY
SOLAR WIND
THREE-DIMENSIONAL CALCULATIONS