The input of local source information and propagation parmeters at a scale of O(10) pc are necessary in order to accurately repeat the large scale 2D anisotropy of cosmic ray from TeV to PeV. However, simulating the CR propagation using the normal finite-difference method (FDM) with O(10) pc grids would occupy too much memory and thus could not be performed in usual servers. To solve this problem, we suggested a non-uniform-grid method to allow a set of fine enough grids in vicinity of the solar system. In this work, besides the decription and validation of the method, our calculation successfully explains the observed transition of 2D cosmic ray anisotropy map between TeV and PeV energies.