Interplanetary magnetic field structure and solar wind parameters as inferred from solar magnetic field observations and by using a numerical 2-D MHD model

Details Interplanetary magnetic field structure and solar wind parameters as inferred from solar magnetic field observations and by using a numerical 2-D MHD model Interplanetary magnetic field structure and solar wind parameters as inferred from solar magnetic field observations and by using a numerical 2-D MHD model

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..143..345u&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 143, no. 2, p. 345-363.

Physics

9

Interplanetary Magnetic Fields, Solar Corona, Solar Magnetic Field, Solar Wind, Two Dimensional Models, Magnetohydrodynamics, Solar Rotation

Scientific paper

A numerical, self-consistent MHD simulation is used to determine the parameters of the solar corona and the solar wind. Observations of the large-scale magnetic field at the sun are used to find the boundary conditions for the magnetic field. The planar model used for the solar wind flow consists of two regions. Region I, covering the distance from the solar surface to 10 solar radii, is the region of transonic flow. Region II extends from 10 solar radii to the earth's orbit, and is the region of supersonic, super-Alfvenic flow. Region I is treated as a mixed initial-boundary value problem. For region II, solar rotation is taken into consideration, so that the interaction between fast and slow solar wind streams is treated self-consistently. The calculated solar wind velocity, radial magnetic field, and number density are compared with space-based observations.

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