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Interplanetary stream magnetism - Kinematic effectsThe 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.
Document ID
19760037064
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Burlaga, L. F.
(NASA Goddard Space Flight Center Laboratory for Extraterrestrial Physics, Greenbelt, Md., United States)
Barouch, E.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 8, 2013
Publication Date
January 1, 1976
Publication Information
Publication: Astrophysical Journal
Volume: 203
Subject Category
Astrophysics
Accession Number
76A20030
Distribution Limits
Public
Copyright
Other

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