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

被引：11

作者：

Bobik, P. ^{[1
]}

Boella, G. ^{[2
]}

Boschini, M. J. ^{[2
,3
]}

Consolandi, C. ^{[2
,4
]}

Della Torre, S. ^{[2
,5
]}

Gervasi, M. ^{[2
,4
]}

Grandi, D. ^{[2
]}

Kudela, K. ^{[1
]}

Pensotti, S. ^{[2
,4
]}

Rancoita, P. G. ^{[2
]}

Rozza, D. ^{[2
,5
]}

Tacconi, M. ^{[2
,4
]}

机构：

[1] Inst Expt Phys, Kosice 04001, Slovakia

[2] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy

[3] CINECA, Segrate, MI, Italy

[4] Univ Milano Bicocca, Dept Phys, I-20126 Milan, Italy

[5] Univ Insubria, Dept Sci & High Tecnol, I-22100 Como, Italy

来源：

ADVANCES IN ASTRONOMY | 2013年 / 2013卷

关键词：

MONTE-CARLO APPROACH; SOLAR MODULATION; DRIFT; DIFFUSION; COEFFICIENTS; PROPAGATION; TRANSPORT; PROTONS; SHEET; SOUTH;

D O I：

10.1155/2013/793072

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.. is 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 spacecra. during 1995, can be affected by the modification of the IMF in the polar regions.

引用

页数：12

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