彗星雲の起源と進化

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1) Pulkkinen A., Kataoka R., 2006, Geophys. Res. Lett.
33, L12108
2) ³´8µ 2006, ISAS ¶·.
302, 1
3) Reeves G. D., et al., 2003, Geophys. Res. Lett. 30(10),
1529
4) 9: ¸ 2006, ;¡ 99 ,205
5) <=¹º 2005, ;¡ 98, 409
6) Richardson I. G., et al., 2006, J. Geophys. Res. 111, A
07S09
7) Baker D. N., et al., 1990, J. Geophys. Res. 95, 15133
8) Miyoshi Y., Kataoka R., 2005, Geophys. Res. Lett. 32,
L21105
9) Kataoka R., Miyoshi Y., 2006, Space Weather, 4,
SO9004
Space Weather Forecast of Radiation Belt
Electrons
Ryuho KATAOKA and Yoshizumi MIYOSHI
Solar-Terrestrial Environment Laboratory, Nagoya
University, Furo-cho, Chikusa-ku, Nagoya 464ῌ
8601, Japan
Abstract : Radiation belts show various patterns
of evolution during a few days after a magnetic
storm onset, and the prediction has been a
di$cult problem. Using a 10 year data set of the
sun, solar wind, radiation belts, and geomagnetic
field, we show that the outer radiation belt tends
to be more dangerous for geosynchronous
satellites than usual during storms associated
with coronal holes, and that the outer radiation
belt tends to be rather safe during storms
associated with coronal mass ejections. In this
paper, we report our new findings and introduce
a practical aspect of space weather forecasting of
radiation belts for secure satellite operations.
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