Mathematics
Scientific paper
Apr 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979stin...7928110p&link_type=abstract
Unknown
Mathematics
Gas Streams, Hydrodynamics, Rotating Plasmas, Solar Corpuscular Radiation, Solar Wind, Three Dimensional Flow, Three Dimensional Models, Gas Dynamics, Interplanetary Magnetic Fields, Inviscid Flow, Kinematics, Mathematical Models
Scientific paper
Theoretical aspects of corotating solar wind dynamics on a global scale are explored by means of numerical simulations executed with a nonlinear, inviscid, adiabatic, single-fluid, three-dimensional (3-D) hydrodynamic formulation. A simple, hypothetical 3-D stream structure is defined on a source surface located at 35 solar radius and carefully documents its evolution to 1 AU under the influence of solar rotation. By manipulating the structure of this prototype configuration at the source surface, it is possible to elucidate the factors most strongly affecting stream evolution: (1) the intrinsic correlations among density, temperature, and velocity existing near the source; (2) the amplitude of the stream; (3) the longitudinal breadth of the stream; (4) the latitudinal breadth of the stream; and (5) the heliographic latitude of the centroid of the stream.
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