We apply a 2D Hoop-model to simulate the solar-cycle variation of anomalous and galactic cosmic rays (ACRs and GCRs) in a full 22-year cycle. Our axially symmetric model is 2D, but still captures the waviness of the heliospheric currents sheet (HCS). The strength of the heliospheric magnetic field (HMF), the corresponding diffusion coefficients and the waviness of the HCS are changed continuously. Special attention will be given to the effects of particle drifts, some theoretical and computational aspects will be discussed, including the handling and modifying the magnetic field in the polar regions of the Heliosphere. We also address the apparent disparity of ACRs and GCRs in the recent weak solar cycles when GCRs reached record high intensities while ACRs remained well below their previous intensity maxima. We find that, in addition to the faster diffusion,the weaker HMF and lower equator-to-pole potential, in itself, can also significantly lower the maximum energy ACRs can gain at the termination shock (TS). Also addressed is the distribution of the ACRs in the sectored and unipolar regions at and beyond the termination shock (TS).