Abstract
We discuss magnetic field generation in weakly ionized turbulent gas. We consider the case of nonzero mean magnetic field. We assume that fluctuations are isotropic, and derive evolution equation for pair correlation function of magnetic fluctuations. Stationary solution of this equation is presented.
Highlights
The standard theory of cosmic rays (CR) formation suggests that primary CR consist mainly of protons and contain no antimatter
We look for stationary solutions of Eq (47) with small but nonzero mean magnetic field
The main result of our paper is taking into account the mean magnetic field, and derivation of evolution equations for anisotropic correlators bb
Summary
The standard theory of cosmic rays (CR) formation suggests that primary CR consist mainly of protons and contain no antimatter During their propagation in the Galaxy primary CR interact with protons of galactic gas, resulting in production of secondary CR, including antiprotons and positrons. Recent antimatter observations by PAMELA satellite detected an excess of positrons with energies 10 − 100 GeV (Adriani et al 2009) In this range, the ratio e+/(e− + e+) is about 10% and increases with energy. Several theoretical explanations for this effect were proposed, among them the positrons generation in pulsars and in the annihilation process of dark matter particles Another mechanism for the positrons generation in the Galaxy is possible, that is acceleration of charged particles in giant molecular clouds and secondary CR production there. This mechanism was discussed by Dogiel et al (1987, 2005), long before the launch of the PAMELA satellite in 2006
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