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| Titel |
Occurrence rate of magnetic holes between 0.72 and 1 AU: comparative study of Cluster and VEX data |
| VerfasserIn |
O. A. Amariutei, S. N. Walker, T. L. Zhang |
| Medientyp |
Artikel
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| Sprache |
Englisch
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| ISSN |
0992-7689
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| Digitales Dokument |
URL |
| Erschienen |
In: Annales Geophysicae ; 29, no. 5 ; Nr. 29, no. 5 (2011-05-02), S.717-722 |
| Datensatznummer |
250017007
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| Publikation (Nr.) |
 copernicus.org/angeo-29-717-2011.pdf |
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| Zusammenfassung |
| Localised depressions in the magnetic field magnitude, or magnetic holes, are
common features in many regions of solar system plasma. Two distinct
mechanisms for their generation have been proposed. The first proposed that
the structures are generated locally, close to the point of observation. The
alternative has been proposed by Russell et al.
(2008), who suggest that the
observed magnetic holes represent nonlinear mirror structures that can be
carried by the solar wind over vast distances of mirror stable plasma.
According to Russell et al.
(2008), magnetic holes are created in the vicinity of
the sun and are convected by the solar wind outward. Periods of Cluster 1 and
VEX data when both spacecraft were connected by the solar wind flow have been
considered in this study, in order to determine the evolution of the magnetic
holes occurrence rate. The comparison of the magnetic holes occurrence near
the Venus and the Earth supports the Russell et al.
(2008) premise that they are
generated closer to the Sun most likely somewhere within the orbit of
Mercury. |
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