1.7 Year Quasi-Periodicity in Cosmic Ray Intensity Variation

Details 1.7 Year Quasi-Periodicity in Cosmic Ray Intensity Variation 1.7 Year Quasi-Periodicity in Cosmic Ray Intensity Variation

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....6.3739k&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

Scientific paper

It has been reported previously that ˜ 1.7 year quasi-p erio dicity is seen in cosmic ray intensity variation observed at several Neutron Monitors (NMs) and Voyager spacecrafts by using of wavelet transform technique. We have extended cosmic ray energy by using of muon data and confirm that the quasi-p erio dicity exists. The time evolution of the quasi-p erio dic component shows its peak in 1987. Comparing wavelet power of NMs with maximums in 1982 and 1990, there is one peak for the energy region between two peaks for NMs. Additionally, wavelet power spectrum of the recurrent component was examined for the solar cycle 19, 20, 21 and 22 by using of Climax NM data. The result indicates that the quasi-p erio dicity is more importantly contributing to cosmic ray intensity variation during the cycle 21 than the cycle 19. Introduction Previous studies clarified the existence of periodicity longer than the diurnal component in several space plasma parameters and cosmic ray intensity variations (e.g. Valdes-Garicia et al.[1] , Mursula and Zieger[2] ). Recently, wavelet transform technique has been intro duced to analyse periodicities in cosmic ray intensity variations. Kudela et al.[3] reported relative dominance of ˜ 1.7 and ˜ 1.3year quasi-p erio dicity during the solar cycles 21 and 22, respectively, to other cycles by using of several Neutron Monitors (NMs). Kato et al.[4][5] reported that the general trend of the quasi-p erio dicity is similar between low energy (70 MeV/n) and a few GeV particles observed at Voyager spacecrafts and NMs, respectively. It is natural to be curious about the time evolution of these quasi-p erio dic component in higher energy. In this paper, we report the result of wavelet analysis of the ˜ 1.7 year quasi-p erio dicity in higher energy data observed by the Nagoya muon telescope.

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