A Three-Dimensional Ray-Tracing Study of R-X Mode Waves during High Geomagnetic Activity
XIAO Fu-Liang1, CHEN Lun-Jin2, ZHENG Hui-Nan2, WANG Shui2, GUO Jun3
1School of Physics and Electronic Sciences, Changsha University of Science and Technology, Changsha 4100762Key Laboratory for Basic Plasma Physics of Chinese Academy of Sciences, School of Earth and Space Sciences, University of Science and Technology of China, Hefei 2300263School of Mathematics and Physics, Qingdao University of Science and Technology, Qingdao 266061
A Three-Dimensional Ray-Tracing Study of R-X Mode Waves during High Geomagnetic Activity
1School of Physics and Electronic Sciences, Changsha University of Science and Technology, Changsha 4100762Key Laboratory for Basic Plasma Physics of Chinese Academy of Sciences, School of Earth and Space Sciences, University of Science and Technology of China, Hefei 2300263School of Mathematics and Physics, Qingdao University of Science and Technology, Qingdao 266061
摘要We further present a three-dimensional (3D) ray-tracing study on the propagation characteristic of the superluminous R-X mode waves during high geomagnetic activity following our recent two-dimensional results [J. Geophys. Res. 112(2007)A10214]. We perform numerical calculations for this mode which originates at specific altitude r=2.0RE in the source cavity along a 70° night geomagnetic field line. We demonstrate that the ray path of the R-X mode is essentially governed by the azimuthal angle of the wave vector k. Ray paths starting with azimuthal angle 180° (or in the meridian plane) can reach the lowest latitude, but stay at relatively higher latitudes with the azimuthal angles other than 180° (or off the meridian plane). The results further supports the previous finding that the R-X mode may be physically present in the radiation belts under appropriate conditions.
Abstract：We further present a three-dimensional (3D) ray-tracing study on the propagation characteristic of the superluminous R-X mode waves during high geomagnetic activity following our recent two-dimensional results [J. Geophys. Res. 112(2007)A10214]. We perform numerical calculations for this mode which originates at specific altitude r=2.0RE in the source cavity along a 70° night geomagnetic field line. We demonstrate that the ray path of the R-X mode is essentially governed by the azimuthal angle of the wave vector k. Ray paths starting with azimuthal angle 180° (or in the meridian plane) can reach the lowest latitude, but stay at relatively higher latitudes with the azimuthal angles other than 180° (or off the meridian plane). The results further supports the previous finding that the R-X mode may be physically present in the radiation belts under appropriate conditions.
XIAO Fu-Liang; CHEN Lun-Jin;ZHENG Hui-Nan;WANG Shui;GUO Jun. A Three-Dimensional Ray-Tracing Study of R-X Mode Waves during High Geomagnetic Activity[J]. 中国物理快报, 2008, 25(1): 340-343.
XIAO Fu-Liang, CHEN Lun-Jin, ZHENG Hui-Nan, WANG Shui, GUO Jun. A Three-Dimensional Ray-Tracing Study of R-X Mode Waves during High Geomagnetic Activity. Chin. Phys. Lett., 2008, 25(1): 340-343.
[1] Xiao F L, Chen L J, Zheng H N and Wang S 2007 J.Geophys. Res. 112 A10214 [2] Xiao F L, Chen L X, Zhou Q H, He H Y and Wen Y J 2007 Chin. Phys. Lett. 24 294 [3] Wang D Y 2003 Chin. Phys. Lett. 20 533 [4] Wang D Y, Huang G L and Lu Q M 2004 Chin. Phys.Lett. 21 1997 [5] Lu Q M, Wang L Q, Zhou Y and Wang S 2004 Chin. Phys.Lett. 21 129 [6] Xiao F L, Zhou Q H, Zheng H N and Wang S 2006 J.Geophys. Res. 111 A08208 [7] Xiao F L, Zhao H and He H Y 2006 Chin. Phys. Lett. 23 267 [8] Xiao F L, Zhou Q H, Zheng H N and Wang S 2007 J.Geophys. Res. 112 A07219 [9] Xiao F L, Zheng H N and Wang S 2005 Chin. Phys.Lett. 22, 1552 [10] Xiao F L, Zheng H N and Wang S 2005 Chin. Phys.Lett. 22 517. [11] Xiao F L, Zhao H and He H Y 2005 Chin. Phys. Lett. 22 2451 [12] Xiao F L, He H Y, Zhou Q H, Zheng H N and Wang S 2006 J. Geophys. Res. 111 A11201 [13] Summers D, Thorne R M and Xiao F L 2001 J. Geophys.Res. 106 10853 [14] Green J L, Boardsen S, Garcia L, Taylor W W L, Fung S Fand Reinisch B W 2005 J. Geophys. Res. 110 A03201 [15] Ergun R E, Carlson C W, McFadden J P, Mozer F S, Delory GT, Peria W, Chaston C C, Temerin M, Elphic R, Strangeway R, PfaffR, Cattell C A, Klumpar D, Shelly E, Peterson W, Moebius E andKistler L 1998 Geophys. Res. Lett. 25 2061 [16]Hashimoto K 1984 J. Geophys. Res. 89 7459 [17] Hanasz J, Panchenko M, de Feraudy H, Schreiber R andMogilevsky M M 2003 J. Geophys. Res. 108 1408 [18] Mutel R L Gurnett D A and Christopher I W 2004 Ann. Geophys. 22 2625 [19] Suchy K 1981 Radio Sci. 16 1179 [20] Horne R B 1989 J. Geophys. Res. 94 8895 [21] Chen L J, Zheng H N, Xiao F L and Wang S 2006 Chin. Phys. Lett. 23 2613 [22] Menietti J D and Lin C S 1986 J. Geophys. Res. 91 13559 [23] Hashimoto K, Kudo S and Matsumoto H 1998 J.Geophys. Res. 103 23475 [24]Gallagher D L, Craven P D and Comfort R H 2000 J.Geophys. Res. 105 18819 [25] Wu C S and Lee L C 1979 Astrophys. J. 230621
2008, Vol. 25 
