We present a simple model to show that the spectral slopes of large-scale turbulent magnetic fields in young supernova remnants (SNRs) can be derived from spatial correlation analysis of the polarized synchrotron intensities. The statistical nature of the polarized synchrotron emission is spatially variable owing to the shell-like geometry of the SNR. Setting a synthetic shell that contains two types of turbulent magnetic fields, we analyze the spatial correlations between polarized synchrotron signals from the shell. We find that the correlations that are evaluated at points along the concentric circular-arc of the shell projected onto the sky can recover the spectral slope of given turbulent magnetic fields.