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The spatial-dependent-propagation (SDP) model with a nearby source works wellto reproduce the coevolving features of both cosmic-ray (CR)-nuclei spectra andanisotropy. However, it is well known that the Sun is actually deviating fromthe galactic disk. This will lead to a dominating anisotropy in the directionperpendicular to the galactic disk, which is discrepant with currentobservations. Thus, it is necessary to further investigate the effect of thesolar offset on anisotropy. In this work, to the best of our knowledge, this isthe first time that the combined studies of the solar offset, nuclei spectra,and anisotropy have been performed based on the SDP model. As a result, toreproduce CR spectra and anisotropy, the thickness of the inner halo $(Z_{IH})$ needs to increase linearly with the displacement of the Sun. We alsoknow that the PeV anisotropy could be used to estimate the value of thediffusion coefficient, thus breaking the degeneracy between the diffusioncoefficient and halo thickness. Therefore, it is a good approach to constrainthe halo thickness. Moreover, the anisotropy in the PeV energy region, as a newprobe, might also shed new light on constraining the solar offset. It is hopedthat the anisotropy of the energies from $\rm \sim$TeV to $\rm PeV$ can befinely measured with the LHAASO experiment, leading to a better understandingof the thick halo.

Constraining the Thickness of the Galactic Halo through Cosmic-Ray Anisotropy Using the Spatial-Dependent-Propagation Model