Reply [to “Comment on ‘Periodicities in the interplanetary magnetic field polarity’ by A. L. C. Gonzalez and W. D. Gonzalez”]

1988 ◽  
Vol 93 (A5) ◽  
pp. 4142 ◽  
Author(s):  
W. D. Gonzalez ◽  
A. L. C. Gonzalez
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Field Polarity

Interplanetary Magnetic Field Polarity and the Size of Low-Pressure Troughs Near 180 W Longitude

Science ◽  
1979 ◽  
Vol 204 (4388) ◽  
pp. 60-62 ◽  
Author(s):  
J. M. WILCOX ◽  
P. B. DUFFY ◽  
K. H. SCHATTEN ◽  
L. SVALGAARD ◽  
P. H. SCHERRER ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Low Pressure ◽  
Field Polarity

scholarly journals Latitudinal Dependence of Cosmic Rays Modulation at 1 AU and Interplanetary Magnetic Field Polar Correction

2013 ◽  
Vol 2013 ◽  
pp. 1-12 ◽  
Author(s):  
P. Bobik ◽  
G. Boella ◽  
M. J. Boschini ◽  
C. Consolandi ◽  
S. Della Torre ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Monte Carlo ◽  
Cosmic Rays ◽  
Interplanetary Magnetic Field ◽  
Latitudinal Gradients ◽  
Solar Modulation ◽  
Polar Regions ◽  
Monte Carlo Code ◽  
Field Polarity ◽  
The Imf

The cosmic rays differential intensity inside the heliosphere, for energy below 30 GeV/nuc, depends on solar activity and interplanetary magnetic field polarity. This variation, termed solar modulation, is described using a 2D (radius and colatitude) Monte Carlo approach for solving the Parker transport equation that includes diffusion, convection, magnetic drift, and adiabatic energy loss. Since the whole transport is strongly related to the interplanetary magnetic field (IMF) structure, a better understanding of his description is needed in order to reproduce the cosmic rays intensity at the Earth, as well as outside the ecliptic plane. In this work an interplanetary magnetic field model including the standard description on ecliptic region and a polar correction is presented. This treatment of the IMF, implemented in the HelMod Monte Carlo code (version 2.0), was used to determine the effects on the differential intensity of Proton at 1 AU and allowed one to investigate how latitudinal gradients of proton intensities, observed in the inner heliosphere with the Ulysses spacecraft during 1995, can be affected by the modification of the IMF in the polar regions.

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