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Recent papers have suggested that the slow solar wind is a super-position of material which is released by reconnection from
large coronal loops. This reconnection process is driven by large-scale motions of solar magnetic flux driven by the non-radial
expansion of the solar wind from the differentially rotating photosphere into more rigidly rotating coronal holes.
The elemental composition of the slow solar wind material is observed to be fractionated and more variable than the fast solar
wind from coronal holes. Recently, it has also been reported that fractionation also occurs in 3He/4He. This may be interpreted
in the frame-work of an existing model for fractionation on large coronal loops in which wave-particle interactions preferentially
heat ions thereby modifying their scale-heights.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
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Jean-Claude Hénoux 《Space Science Reviews》1998,85(1-2):215-226
In this review, the main models of ion-neutral frationation leading to an enhancement of the low FIP to high FIP abundance
ratio in the corona or in the solar wind, are presented. Models based on diffusion parallel to the magnetic field are discussed;
they are highly dependent on the boundary conditions. The magnetic field, that naturally separates ions from neutrals moving
perpendicular to the field lines direction, when the ion-neutral frequency becomes lower than the ion gyrofrequency, is expected
to play an active role in the ion-neutral separation. It is then suggested that ion-neutral fractionation is linked to the
formation of the solar chromosphere, i.e. in magnetic flux-tubes at a temperature between 4000 and 6000 K.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
3.
T. H. Zurbuchen S. Hefti L. A. Fisk G. Gloeckler R. Von Steiger 《Space Science Reviews》1999,87(1-2):353-356
The transition between coronal hole associated fast solar wind and slow solar wind is studied using data from the high resolution
mass spectrometer SWICS on ACE. We discuss the data in the framework of a recent theory about the global heliospheric magnetic
field and conclude that the data are consistent with magnetic connections between field-lines in the fast and in the slow
wind.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
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