Mathematics – Probability
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010eguga..1213622a&link_type=abstract
EGU General Assembly 2010, held 2-7 May, 2010 in Vienna, Austria, p.13622
Mathematics
Probability
Scientific paper
We study a relationship between the interplanetary magnetic field (IMF) and the solar wind speed (SWS) turbulence measured in the interplanetary space (in situ) and the galactic cosmic ray (GCR) intensity fluctuations measured by neutron monitors (at earth surface) for different time scales of ranges 5 - 60 minutes and 1 - 24 hours. We calculate the Probability Distribution Functions (PDF) of differences δB?, δV ? , and δI? of the time series B(ti) of the IMF strength , V (ti) of the SWS, and I(ti) of the GCR intensity, respectively, as δB? = B(t + ?) - B(t), δV ? = V (t + ?) - V (t) and δI? = I(t + ?) - I(t) over varying time scales ?. Then, we find correlation coefficients among them and characteristic time scale ?0 for which (? > ?0) the asymmetry (skewness) and kurtosis of PDFs are minimum, and in good approximation PDFs have Gaussian distributions. We show that the asymmetry and inhomogeneities of the IMF and solar wind turbulence generally are manifested for time scale ? < 1 day, while for the GCR fluctuations for ? ?0, and PDF has a Gaussian distribution, the IMF turbulence is characterized by the power spectral density (PSD), with parameters p and ν (PSD = Pf-ν , where P is power and f is a frequency). In this case diffusion of GCR particles could be described by the quasi linear theory (QLT), and diffusion coefficient K is proportional to the rigidity R, as K ~ R2-ν; correspondingly, the exponent γ of the rigidity R spectrum (δD(R)-D(R) ∞ R-γ) of the GCR intensity variations (e.g. of Forbush decrease) of the energy to which neutron monitors and muon telescopes (for rigidity > 5 - 10 GV) respond, is determined by the exponent ν of PSD of the IMF turbulence.
Alania Michael V.
Modzelewska Renata
Wawrzynczak Anna
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