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The HelMod Monte Carlo Model for the Propagation of Cosmic Rays in Heliosphere

Published online by Cambridge University Press:  24 July 2018

Matteo J. Boschini ,
Stefano Della Torre Open the ORCID record for Stefano Della Torre [Opens in a new window] ,
Massimo Gervasi ,
Davide Grandi ,
Giuseppe La Vacca ,
Simonetta Pensotti ,
Pier Giorgio Rancoita ,
Davide Rozza Open the ORCID record for Davide Rozza [Opens in a new window]  and
Mauro Tacconi
Matteo J. Boschini
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Cineca, Segrate, Italy
Stefano Della Torre
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected]
Massimo Gervasi
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Università degli Studi di Milano Bicocca, I-20126 Milano, Italy
Davide Grandi
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Università degli Studi di Milano Bicocca, I-20126 Milano, Italy
Giuseppe La Vacca
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Università degli Studi di Milano Bicocca, I-20126 Milano, Italy
Simonetta Pensotti
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Università degli Studi di Milano Bicocca, I-20126 Milano, Italy
Pier Giorgio Rancoita
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected]
Davide Rozza
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Università degli Studi di Milano Bicocca, I-20126 Milano, Italy
Mauro Tacconi
Affiliation:
INFN Sezione di Milano Bicocca, I-20126 Milano, Italy email: [email protected] Università degli Studi di Milano Bicocca, I-20126 Milano, Italy
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Abstract

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The heliospheric modulation model HelMod solves the transport-equation for Galactic Cosmic Ray propagation through the heliosphere down to Earth. It is based on a 2-D Monte Carlo approach that includes a general description of the symmetric and antisymmetric parts of the diffusion tensor, thus properly treating the particle drift effects as well as convection within the solar wind and adiabatic energy loss. The model was tuned in order to fit 1) the data observed outside the ecliptic plane at several distances from the Earth and 2) the spectra observed near the Earth for both, high and low solar activity periods. Great importance was given to description of polar regions of the heliosphere. We present the flux for protons, antiprotons and helium nuclei computed for solar cycle 23-24 in comparison with experimental observations and prediction for the full solar cycle 24.

Keywords

Sun: activitycosmic raysdiffusionelementary particlesinterplanetary mediumISM: generalSun: heliospheremethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S335: Space Weather of the Heliosphere: Processes and Forecasts , July 2017 , pp. 276 - 279
Copyright
Copyright © International Astronomical Union 2018 

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