How are Forbush decreases related to interplanetary magnetic field enhancements?

K. P. Arunbabu; H. M. Antia; S. R. Dugad; S. K. Gupta; Y. Hayashi; S. Kawakami; P. K. Mohanty; A. Oshima; P. Subramanian

doi:10.1051/0004-6361/201425115

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Volume 580 (August 2015)

A&A, 580 (2015) A41

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Issue		A&A Volume 580, August 2015


Article Number		A41
Number of page(s)		13
Section		The Sun
DOI		https://doi.org/10.1051/0004-6361/201425115
Published online		24 July 2015

Online material

Appendix A: Additional figures

	Fig. A.1 FD event of 11 April 2001 and magnetic field for nine directions in GRAPES-3 muon telescope. The linestyles are the same as used in Fig. 2.
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	Fig. A.2 FD event of 23 May 2002 and magnetic field for nine directions in GRAPES-3 muon telescope. The linestyles are the same as used in Fig. 2.
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	Fig. A.3 FD event on 11 April 2001. The linestyles are the same as used in Fig. 5.
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	Fig. A.4 FD event on 23 May 2002. The linestyles are the same as used in Fig. 5.
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Fig. A.5

Cross correlation of the cosmic ray flux with B_total. The top panel shows the percentage deviation of cosmic ray flux using solid black lines and the magnetic field using dotted black lines (scaled to fit in the frame). The middle panel shows the same with magnetic field shifted to the right corresponding to the time lag and the bottom panel shows the correlation coefficient for different lags.

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Fig. A.6

Cross correlation of the cosmic ray flux with B_total. The top panel shows the percentage deviation of cosmic ray flux using solid black lines and the magnetic field using dotted black lines (scaled to fit in the frame). The middle panel shows the same with magnetic field shifted to the right corresponding to the time lag and the bottom panel shows the correlation coefficient for different lags.

Open with DEXTER

Appendix B: Additional Tables

Table B.1

FD events for which the correlation coefficient between the profiles of the FD and the IMF enhancement ≥70%.

Table B.2

Number of diffusions required for the observed lag in FD events using three different turbulent spectrums and two different methods described in Sect. 7.

© ESO, 2015

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