Kozlov V I, Markov V V. 2007. Wavelet image of a heliospheric storm in cosmic rays. Geomagnetism and Aeronomy, 47(1): 52-61.
[2]
Kudela K, Storini M, Antalova A, et al. 2001. On the wavelet approach to cosmic ray variability. Proceedings of the 27th ICRC, 3773.
[3]
Le G M, Ye Z H, Yu S H, et al. 2004. Wavelet analysis of the cosmic ray intensities at Guangzhou muon station during January 7-11, 1997. Chinese J. Geophys. (in Chinese), 47(2): 190-194.
[4]
Liu J, Zhou D W. 2007. Application of wavelets analysis in the variation of cosmic ray with time. Journal of Henan Institute of Education (Natural Science) (in Chinese), 16(2): 9-11.
[5]
Xue B S, Ye Z H, Gong J H. 2007. Preliminary attempt in prediction the geomagnetic storm with ground cosmic ray data. Chin. J. Space Sci. (in Chinese), 27(3): 218-222.
[6]
Zarrouk N, Bennaceur R. 2009. A wavelet based analysis of cosmic rays modulation. Acta Astronautica, 65(1-2): 262-272.
[7]
Belov A V, Dorman L I, Eroshenko E A, et al.1995. Anisotropy of cosmic rays and Forbush decreases in 1991.//Proceedings of 24th International Cosmic Ray Conference, 4: 912-914.
[8]
Caswell J M. 2014. Combination of wavelet analysis and artificial neural networks applied to forecast of daily cosmic ray impulses. International Letters of Chemistry, Physics and Astronomy, 34: 55-63.
[9]
Chowdhury P. 2011. Study on solar and cosmic ray activities and their periodic behaviour.//Proceedings of the 29th Meeting of the ASI Conference Series, Vol. 3, 69-74.
[10]
Dorman L. 1965. Variation of Cosmin Ray (in Chinese). Beijing: Science Press.
[11]
Dorman L I, Libin I Y. 1984. Cosmic-ray scintillations and dynamic processes in space. Space Sci. Rev., 39(1-2): 91-152.
[12]
Farge M. 1992. Wavelet transforms and their applications to turbulence. Annual Review of Fluid Mechanics, 24(1): 395-458.
[13]
Grinsted A, Moore J C, Jevrejeva S. 2004. Application of the cross wavelet transform and wavelet coherence to geophysical time series. Nonlinear Processes in Geophysics, 11(5-6): 561-566.
[14]
Kim K H, Moon Y J, Cho K S. 2007. Prediction of the 1-AU arrival times of CME-associated interplanetary shocks: Evaluation of an empirical interplanetary shock propagation model. J. Geophys. Res., 122(A5), doi: 10.1029/2006JA011904.
[15]
Kozlov V I, Tugolukov N. 1992. Intensity scintillations of cosmic rays. I-Verification. Aeron, 32: 153-156.
[16]
Miao J, Xue B S, Ye Z H. 2003. The wavelet character of cosmic ray intensity before geomagnetic stroms. Chin. J. Space Sci. (in Chinese), 23(6): 452-458.
[17]
Morozova E I, Pissarenko N F, Riedler W, et al. 1984. The magnetic field turbulence near interplanetary shock fronts. Advances in Space Research, 4(2-3): 331-334.
[18]
Owens A J, Jokipii J R. 1974. Cosmic Ray Scintillations: 3. The low-frequency limit and observations of interplanetary scintillations. J. Geophys. Res., 79(7): 907-912.
[19]
Pérez-Peraza J, Leyva-Contreras A, Libin I Y. 1998. Prediction of interplanetary shock waves using cosmic ray fluctuations. Geofísica Internacional, 37(2): 87-93.
[20]
Richardson I G, Dvornikov V M, Sdobnov V E, et al. 2000. Bidirectional particle flows at cosmic ray and lower (~1 MeV) energies and their association with interplanetary coronal mass ejections/ejecta. J. Geophys. Res, 105(A6): 12579-12591.
[21]
Sakai T, Kato M, Takei R, et al. 1985. Periodic variations of cosmic ray intensity with period of about 37 minutes observed on April 25th, 1984. J. Geomagn. Geoelectr., 37(6): 659-666.
[22]
Tu C Y. 1988. Solar Terriscial Physics(in Chinese). Beijing: Science Press.
[23]
Torrence C, Compo G P. 1998. A practical guide to wavelet analysis. Bulletin of the American Meteorological Society, 79(1): 61-78.
[24]
Torrence C, Webster P J. 1999. Interdecadal Changes in the ENSO-Monsoon system. Journal of Climate, 12(8): 2679-2690.
[25]
Wang J, Liu S Q, Xue B S, et al. 2009. Anisotropy analyses of cosmic ray before the geomagnetic storm on Sep. 24, 1998. Chin. J. Space Sci. (in Chinese), 29(5): 495-501.
[26]
Wang Y M, Ye P Z, Wang S, et al. 2001. A statistical study on the geoeffectiveness of Earth-directed coronal mass ejections from March 1997 to December 2000. J. Geophys. Res., 107(A11): SSH 2-1-SSH 2-9.
[27]
Wang Y M, Zhang B, Guo L X, et al. 2011. Cross wavelet analysis and R/S analysis of relationship between geomagnetic Ap index and sunspot number. Scientia Geographica Sinica (in Chinese), 31(6): 747-752.
[28]
Webb D F. 2002. CMEs and the solar cycle variation in their geoeffectiveness.//Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 409-419.