ULF Waves Associated with Solar Wind Deceleration in the Earth's Foreshock
FU Hui-Shan1,2, CAO Jin-Bin3,1, YANG Biao4, Lucek E5, Rème H6, Dandouras I6
1State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Beijing 1001902Graduate University of Chinese Academy of Sciences, Beijing 1000493Beijing University of Aeronautics and Astronautics, Beijing 1001904Institute of Space Physics and Applied Technology, Peking University, Beijing 1008715Blackett Laboratory, Imperial College, Prince Consort Road, London, SW7 2BZ, UK6Centre d'Etude Spatiale des Rayonnements, 31028, Toulouse, France
ULF Waves Associated with Solar Wind Deceleration in the Earth's Foreshock
FU Hui-Shan1,2, CAO Jin-Bin3,1, YANG Biao4, Lucek E5, Rème H6, Dandouras I6
1State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Beijing 1001902Graduate University of Chinese Academy of Sciences, Beijing 1000493Beijing University of Aeronautics and Astronautics, Beijing 1001904Institute of Space Physics and Applied Technology, Peking University, Beijing 1008715Blackett Laboratory, Imperial College, Prince Consort Road, London, SW7 2BZ, UK6Centre d'Etude Spatiale des Rayonnements, 31028, Toulouse, France
摘要Characteristics of ULF waves associated with the solar wind deceleration in the Earth's foreshock on 6-7 April 2003 is studied using the wave telescope technique. In the satellite frame, the ULF waves are the left-handed polarized and quasi anti-parallel propagating mode, with a power peak at about 18.63mHz. The wave vector in the GSE coordinates is estimated to be k = (-4.29, 2.28, 1.21)×10-4km-1. In the solar wind frame, the frequency of waves becomes -9.39mHz after the Doppler shift correction. The propagation direction of the waves is thus reversed and correspondingly the polarization of the waves becomes right-handed. The above-mentioned characteristics of the ULF waves in the solar wind frame indicate that the ULF waves associated with the solar wind deceleration are the Alfven-whistler waves, which have been frequently reported in both the observations and computer simulations.
Abstract：Characteristics of ULF waves associated with the solar wind deceleration in the Earth's foreshock on 6-7 April 2003 is studied using the wave telescope technique. In the satellite frame, the ULF waves are the left-handed polarized and quasi anti-parallel propagating mode, with a power peak at about 18.63mHz. The wave vector in the GSE coordinates is estimated to be k = (-4.29, 2.28, 1.21)×10-4km-1. In the solar wind frame, the frequency of waves becomes -9.39mHz after the Doppler shift correction. The propagation direction of the waves is thus reversed and correspondingly the polarization of the waves becomes right-handed. The above-mentioned characteristics of the ULF waves in the solar wind frame indicate that the ULF waves associated with the solar wind deceleration are the Alfven-whistler waves, which have been frequently reported in both the observations and computer simulations.
FU Hui-Shan;CAO Jin-Bin;YANG Biao;Lucek E;Rème H;Dandouras I. ULF Waves Associated with Solar Wind Deceleration in the Earth's Foreshock[J]. 中国物理快报, 2009, 26(11): 119402-119402.
FU Hui-Shan, CAO Jin-Bin, YANG Biao, Lucek E, Rème H, Dandouras I. ULF Waves Associated with Solar Wind Deceleration in the Earth's Foreshock. Chin. Phys. Lett., 2009, 26(11): 119402-119402.
[1] Formisano V and Amata E 1976 J. Geophys. Res. 81 3907 [2] Bame S J et al 1980 J. Geophys. Res. 85 2981 [3] Bonifazi C et al 1980 J. Geophys. Res. 85 6031 [4] Zhang~T L et al 1995 Adv. Space Res. 10 137 [5] Auer R D et al 1976 J. Geophys. Res. 81 2030 [6] Diodato L and Moreno G 1977 J. Geophys. Res. 82 3615 [7] Cao J B et al 2009 J. Geophys. Res. 114 A02207 [8] Fu H S et al 2009 Chin. J. Geophys. 52 895 [9] Le G and Russell C T 1990 Geophys. Res. Lett. 17 905 [10] Le G et al 1992 J. Geophys. Res. 97 2917 [11] Greenstadt E W et al 1995 Adv. Space Res. 1571 [12] Blanco-Cano X et al 1995 Adv. Space Res. 1597 [13] Blanco-Cano X et al 1997 Ann. Geophys. 15 273 [14] Blanco-Cano X et al 1999 J. Geophys. Res. 1044643 [15] Blanco-Cano X at al 2006 J. Geophys. Res. 111A10205 [16] Mazelle C et al 1997 Adv. Space Res. 20 267 [17] Pin\c{con J L and Lefeuvre F 1991 J. Geophys. Res. 96 1789 [18] Motschmann U et al 1996 J. Geophys. Res. 1014961 [19] Glassmeier K H et al 2001 Ann. Geophys. 191439 [20] Glassmeier K H 2003 Ann. Geophys. 21 1071 [21] Narita Y et al 2003 Geophys. Res. Lett. 301710 [22] Narita Y et al 2005 J. Geophys. Res. 110A12215 [23] Balogh A et al 2001 Ann. Geophys. 19 1207 [24] R\`{eme H et al 2001 Ann. Geophys. 19 1303 [25] Russell C T 1988 Adv. Space Res. 8 147 [26] Wang~X~Y and Lin Y 2003 Physics of Plasmas 103528 [27] Narita Y et al 2007 Nonlin. Processes Geophys. 14 361 [28] Yoon P H 2007 Physics of Plasmas 14 102302 [29] Vogt J et al 2008 Ann. Geophys. 26 1699 [30] Motschmann U et al 1997 Ann. Geophys. 15 603 [31] Cao J B et al 1998 J. Geophys. Res. 103 2055 [32] Cao J B et al 1998 Geophys. Res. Lett. 251499 [33] Cao J B et al 2000 Phys. Plasmas 7 696 [34] Parks G K. et al 2006 Phys. Plasmas 13 050701 [35] Coates A J et al 1993 J. Geophys. Res. 9820985
2009, Vol. 26 
