This paper presents a numerical implementation of the efficient line of sight method to calculate the anisotropy and polarization of the cosmic microwave background (CMB) for scalar and tensor modes in almost-Friedmann-Robertson-Walker (FRW) models with positive spatial curvature. The authors describe a new method for calculating the polarization power spectra in such models, which is essential for understanding the universe's structure and evolution. The method is based on the 1+3 covariant formalism, which provides a physically transparent, exact description of both dynamics and radiative transfer in general cosmological models. The authors use this formalism to implement a numerical code that allows efficient exploration of the full cosmological parameter space. The code is based on the field-tested CMBFAST code, which uses a line of sight integration method to achieve high efficiency without compromising accuracy. The authors present new results for the polarization power spectra from scalar and tensor perturbations in closed models. They also calculate the intensity power spectra in closed models, extending previous semi-analytic predictions. The results show that the intensity quadrupole for tensor modes in the closed model is suppressed relative to the flat model due to the cutoff at ν=3. The authors compare their results with those from CMBFAST version 2.4.1 and a pre-release version of CMBFAST which supports closed models. They find good agreement well into the damping tail. The results are presented in Figure 1, which shows the scalar and tensor intensity and polarization power spectra in closed and flat CDM models. The authors conclude that their method allows accurate and rapid modeling over the full volume of parameter space of FRW models. Their Fortran 90 code is publicly available at http://www.mrao.cam.ac.uk/~aml1005/cmb. The authors are supported by various grants and institutions, and they thank others for their contributions to the work.This paper presents a numerical implementation of the efficient line of sight method to calculate the anisotropy and polarization of the cosmic microwave background (CMB) for scalar and tensor modes in almost-Friedmann-Robertson-Walker (FRW) models with positive spatial curvature. The authors describe a new method for calculating the polarization power spectra in such models, which is essential for understanding the universe's structure and evolution. The method is based on the 1+3 covariant formalism, which provides a physically transparent, exact description of both dynamics and radiative transfer in general cosmological models. The authors use this formalism to implement a numerical code that allows efficient exploration of the full cosmological parameter space. The code is based on the field-tested CMBFAST code, which uses a line of sight integration method to achieve high efficiency without compromising accuracy. The authors present new results for the polarization power spectra from scalar and tensor perturbations in closed models. They also calculate the intensity power spectra in closed models, extending previous semi-analytic predictions. The results show that the intensity quadrupole for tensor modes in the closed model is suppressed relative to the flat model due to the cutoff at ν=3. The authors compare their results with those from CMBFAST version 2.4.1 and a pre-release version of CMBFAST which supports closed models. They find good agreement well into the damping tail. The results are presented in Figure 1, which shows the scalar and tensor intensity and polarization power spectra in closed and flat CDM models. The authors conclude that their method allows accurate and rapid modeling over the full volume of parameter space of FRW models. Their Fortran 90 code is publicly available at http://www.mrao.cam.ac.uk/~aml1005/cmb. The authors are supported by various grants and institutions, and they thank others for their contributions to the work.