The solar modulation, a combination of diffusion, convection, magnetic drift and energy loss inside the heliosphere is usually seen as a depletion in the Galactic cosmic ray (CR) flux at low energy (less than 10 GeV/nuc). Antiparticles such as antiprotons or positrons undergo the same processes of respective particles but with a different magnitude depending on the Solar magnetic field polarity. For electrons and positrons, due to the small mass, energy loss mechanisms as inverse compton, synchrotron, bremsstrahlung and ionization have to be taken into account, together with the typical adiabatic losses considered in the heliosphere. We developed a Monte Carlo stochastic simulation with the aim to compare the solar modulation of particles and antiparticles in the same observation period. We are able to estimate the different behaviours associated to the charge sign dependent processes of the heliospheric modulation. We compared the simulated positron fraction with measurements performed by AMS-01 and PAMELA. We also present the prediction for the AMS-02 experiment.

Bobik, P., Boschini, M., Consolandi, C., Della Torre, S., Gervasi, M., Grandi, D., et al. (2011). Electron and positron solar modulation and prediction for AMS02. In Proceedings of the 12th ICATPP Conference "Cosmic Rays for Particle and Astroparticle Physics" (Villa Olmo, Como, Italy 7-8 October 2010) (pp.337-342). World Scientific Publishing Co. Pte Ltd [10.1142/9789814329033_0043].

Electron and positron solar modulation and prediction for AMS02

CONSOLANDI, CRISTINA;GERVASI, MASSIMO;Grandi, D;PENSOTTI, SIMONETTA;
2011

Abstract

The solar modulation, a combination of diffusion, convection, magnetic drift and energy loss inside the heliosphere is usually seen as a depletion in the Galactic cosmic ray (CR) flux at low energy (less than 10 GeV/nuc). Antiparticles such as antiprotons or positrons undergo the same processes of respective particles but with a different magnitude depending on the Solar magnetic field polarity. For electrons and positrons, due to the small mass, energy loss mechanisms as inverse compton, synchrotron, bremsstrahlung and ionization have to be taken into account, together with the typical adiabatic losses considered in the heliosphere. We developed a Monte Carlo stochastic simulation with the aim to compare the solar modulation of particles and antiparticles in the same observation period. We are able to estimate the different behaviours associated to the charge sign dependent processes of the heliospheric modulation. We compared the simulated positron fraction with measurements performed by AMS-01 and PAMELA. We also present the prediction for the AMS-02 experiment.
paper
cosmic rays; heliosphere; positron ratio; solar modulation
English
ICATPP Conference on Cosmic Rays for Particle and Astroparticle Physics
2010
Giani, S; Leroy, C; Rancoita, PG
Proceedings of the 12th ICATPP Conference "Cosmic Rays for Particle and Astroparticle Physics" (Villa Olmo, Como, Italy 7-8 October 2010)
978-981-4329-02-6
2011
6
337
342
none
Bobik, P., Boschini, M., Consolandi, C., Della Torre, S., Gervasi, M., Grandi, D., et al. (2011). Electron and positron solar modulation and prediction for AMS02. In Proceedings of the 12th ICATPP Conference "Cosmic Rays for Particle and Astroparticle Physics" (Villa Olmo, Como, Italy 7-8 October 2010) (pp.337-342). World Scientific Publishing Co. Pte Ltd [10.1142/9789814329033_0043].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/39060
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