Modeling of the Interstellar Antiproton Flux on the Basis of the Leaky-Box Propagation Model

Details Modeling of the Interstellar Antiproton Flux on the Basis of the Leaky-Box Propagation Model Modeling of the Interstellar Antiproton Flux on the Basis of the Leaky-Box Propagation Model

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh51c..01p&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #SH51C-01

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2720 Energetic Particles: Trapped, 2753 Numerical Modeling, 7807 Charged Particle Motion And Acceleration, 7859 Transport Processes

Scientific paper

Numerous modeling of the galactic antiproton flux originated from interactions of Cosmic Rays with interstellar matter has shown that the calculated flux is lower than the antiproton flux observed near the Earth. To assess this discrepancy, in our modeling we have made an effort to eliminate all possible uncertainties in the parameters of antiproton flux calculation, and we have used modern nuclear reaction computer code accounting for antiparticle behavior. Common uncertainties include the incomplete knowledge of cross sections for antiproton production, the corresponding spectral limitations, the precise knowledge of annihilation and scattering, and the limitations on the antiproton propagation models for the heliosphere. In this presentation we show results of simulation of antiproton (pbar) production in (p,A) and (pbar,A) reactions and the influence of the latter on the interstellar antiproton flux. The antiproton yield was simulated on the basis of nuclear reaction Multy Stage Dynamical Model computer code (Dementyev et al). The interstellar antiproton flux is calculated for the Leaky-box propagation model including accounting for the tertiary antiprotons produced by secondary antiprotons in nuclear reactions with the interstellar gas. Tertiaries were calculated on the base of Tan et al., approximation and using the MSDM code. The tertiary antiproton spectral shape obtained with MSDM approximation differs modestly from the shape with the Tan and Ng approximation. However, this difference affects only the antiproton spectrum at E < 0.1 GeV, i.e. in the energy range where at present direct measurements are absent. The calculated flux was modulated within the heliosphere for periods of minimum and maximum solar activity accordingly to (Moskalenko et al.), and it agrees quite well with the BESS experimental results obtained in the minimum solar activity and also with BESS (2000) results in epoch near the maximum solar activity. Dementyev, A.V. et al., Radiation Measurements, 30, 553, 1999. Tan, L.C.,et al., Phys. Rev., D26, 1179-1182, 1983. Moskalenko, I.V., et al., Ap.J. (565), 280-296, 2002.

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