Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...203..257b&link_type=abstract
Astrophysical Journal, vol. 203, Jan. 1, 1976, pt. 1, p. 257-267.
Astronomy and Astrophysics
Astrophysics
12
Interplanetary Magnetic Fields, Kinetic Theory, Solar Wind, Astronomical Maps, Astronomical Models, Density Distribution, Dynamic Models, Magnetic Flux, Magnetic Measurement, Velocity Distribution
Scientific paper
The particle density and the magnetic-field intensity and direction are calculated for volume elements of the solar wind as a function of the initial magnetic-field direction and the initial speed gradient. It is assumed that the velocity is constant and radial. These assumptions are approximately valid between about 0.1 and 1.0 AU for many streams. Time profiles of the particle density, field intensity, and velocity are calculated for corotating streams, neglecting effects of pressure gradients. The compression and rarefaction of the magnetic field depend sensitively on the initial field direction. By averaging over a typical stream, it is found that the average radial field intensity is inversely proportional to the square of the heliocentric distance, whereas the average intensity in the direction of the planets' motion does not vary in a simple way, consistent with deep space observations. Changes of field direction may be very large, depending on the initial angle; but when the initial angle at 0.1 AU is such that the base of the field line corotates with the sun, the spiral angle is the preferred direction at 1 AU. The theory is also applicable to nonstationary flows.
Barouch E.
Burlaga Leonard Francis
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