  The spatial-dependent propagation (SDP) model with a nearby source works well
to reproduce the co-evolving features of both cosmic ray (CR) nuclei spectra
and anisotropy. However, it is well known that the Sun is offset from the
Galactic plane. This will lead to a dominating anisotropy in perpendicular
direction, which is discrepant with observations. Thus it is necessary to
reboot further investigation into the effect of the solar offset. In this work,
for the first time the combined studies of the solar offset, nuclei spectra and
anisotropy are performed based on the SDP model. As a result, to reproduce CR
spectra and anisotropy, the thickness of the halo $\rm (\xi z_h)$ increases
linearly with the displacement of the Sun. When the offset is $\rm \sim8~pc$ as
estimated from the matter-borne methods, $\rm \xi z_h$ is about 0.9 kpc, which
is a much thicker halo than usually. Moreover, the PeV anisotropy could
estimate the value of diffusion coefficient, thus breaking the degeneracy of
diffusion coefficient and halo thickness. Therefore it is a good messenger to
constrain the halo thickness. On the other hand, the anisotropy in PeV energy
region, as a new probe, might also shed new light to constrain the solar
offset. We hope that the anisotropy at the energies of $\rm \sim TeV$ to $\rm
PeV$ can be finely measured by LHAASO experiment, leading to a better
understanding about the thick halo.
