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Magnetic reconnection is a fundamental process for releasing magnetic energy in space physics and astrophysics. At present, the usual way to investigate the reconnection process is through analytical studies or first-principles numerical simulations. This paper is the first to understand the turbulent magnetic reconnection process by exploring the nature of magnetic turbulence. From the perspective of radio synchrotron polarization statistics, we study how to recover the properties of the turbulent magnetic field by considering the line of sight along different directions of the reconnection layer. We find that polarization intensity statistics can reveal the spectral properties of reconnection turbulence. This work opens up a new way of understanding turbulent magnetic reconnection., Comment: 12 pages, 7 figures, 1 table. Accepted for publication in ApJ

Since synchrotron polarization fluctuations are related to the fundamental properties of the magnetic field, we propose the polarization intensity variance to measure the Galactic interstellar medium (ISM) magnetization. We confirm the method's applicability by comparing it with the polarization angle dispersion and its reliability by measuring the underlying Alfv\'enic Mach number of MHD turbulence. With the finding of the power-law relation of $\mathcal{A} \propto M_{\rm A}^{2}$ between polarization intensity variance $\mathcal{A}$ and Alfv\'enic Mach number $M_{\rm A}$, we apply the new technique to the Canadian Galactic Plane Survey (CGPS) data, achieving Alfv\'enic Mach number of the Galactic ISM. Our results show that the low-latitude Galactic ISM is dominated by sub-Alf\'enic turbulence, with $M_{\rm A}$ approximately between 0.5 and 1.0., Comment: 10 pages, 5 figures, and 2 tables. Accepted for publication in ApJ