CORONAL RADIATION BELTS

被引：4

作者：

Hudson, H. S. ^{[1
]}

MacKinnon, A. L. ^{[2
]}

DeRosa, M. L. ^{[3
]}

Frewen, S. F. N. ^{[1
]}

机构：

[1] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[2] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland

[3] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2009年 / 698卷 / 02期

关键词：

acceleration of particles; Sun: corona; Sun: magnetic fields; GAMMA-RAY EMISSION; MAGNETIC-FIELDS; SOLAR CORONA; ENERGETIC PARTICLES; INTERPLANETARY; FLARE; WIND;

D O I：

10.1088/0004-637X/698/2/L86

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The magnetic field of the solar corona has a large-scale dipole character, which maps into the bipolar field in the solar wind. Using standard representations of the coronal field, we show that high-energy ions can be trapped stably in these large-scale closed fields. The drift shells that describe the conservation of the third adiabatic invariant may have complicated geometries. Particles trapped in these zones would resemble the Van Allen belts and could have detectable consequences. We discuss potential sources of trapped particles.

引用

页码：L86 / L89

页数：4

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