Statistics – Applications
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..152..429f&link_type=abstract
Solar Physics, vol. 152, no. 2, p. 429-444
Statistics
Applications
1
Applications Of Mathematics, Coronal Holes, Magnetic Field Configurations, Magnetohydrodynamic Flow, Magnetohydrodynamic Waves, Mathematical Models, Plasma Control, Solar Magnetic Field, Solar Wind, Solar Wind Velocity, Stellar Models, Correlation Coefficients, Plasma Density, Plasma Temperature, Skylab Program, Statistical Correlation, Wave-Particle Interactions
Scientific paper
In this paper we give an explanation for a control mechanism for velocity V of solar wind (SW) streams for coronal holes (CHs) based on the idea suggested by Rudenko and Fainshtein (1993). In accordance with that idea, the difference of values of V in high-speed SW streams from different CHs is due to the spread in magnitude of magnetic field Ba in the region of acceleration of such streams near the Sun. In this case, with increasing magnitude of Ba, there is an increase in velocity of the high-speed stream. Through calculations of the coronal magnetic field (potential-field approximation) it is shown that on the source surface the magnetic field (Bs), averaged over the cross-section of the magnetic tube from a CH, can vary for different tubes over a wide range and correlates quite well with the area of this tube's base as well as depending on the radial component of the magnetic field at the base of the tube on the source surface (Bor). It is found that the value of superradial divergence of the magnetic tube from a CH depends not only on the area of its base (as shown in prior work) but also on (Bor). A positive correlation at the Earth's orbit between velocity V of the high-speed SW and the radial component of the magnetic field in the region of this stream is detected, which agrees indirectly with the V-control mechanism under discussion.
Fainshtein V.. G.
Kaigorodov A. P.
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