Galactic foreground and CMB emissions randomization due to chaotic/turbulent dynamics of magnetized plasma dominated by magnetic helicity

Abstract: Using results of numerical simulations and astrophysical observations (mainly in the WMAP and Planck frequency bands) it is shown that Galactic foreground emission becomes more sensitive to the mean magnetic field with the frequency, that results in the appearance of two levels of its randomization due to chaotic/turbulent dynamics of magnetized interstellar medium dominated by the magnetic helicity. The galactic foreground emission is more randomized at higher frequencies. The Galactic synchrotron and polarized dust emissions have been studied in detail. It is shown that the magnetic field imposes its level of randomization on the synchrotron and dust emission. The background magnetic field (around the lepto/baryogenesis) and CMB emission have also been briefly discussed in this context. It is shown that they are considerably less randomized than the foreground ones. The main method for the theoretical consideration used in this study is the Kolmogorov-Iroshnikov phenomenology within the framework of the distributed chaos notion. Despite the vast differences in the values of physical parameters and spatio-temporal scales between the numerical simulations and the astrophysical observations, there is a quantitative agreement between the results of the astrophysical observations and the numerical simulations within the framework of the distributed chaos notion.