  Small-scale magnetic fields are not only the fundamental element of the solar
magnetism, but also closely related to the structure of the solar atmosphere.
The observations have shown that there is a ubiquitous tangled small-scale
magnetic field with a strength of 60 $\sim$ 130\,G in the canopy forming layer
of the quiet solar photosphere. On the other hand, the multi-dimensional MHD
simulations show that the convective overshooting expels the magnetic field to
form the magnetic canopies at a height of about 500\,km in the upper
photosphere. However, the distribution of such small-scale ``canopies" in the
solar photosphere cannot be rigorously constrained by either observations and
numerical simulations. Based on stellar standard models, we identify that these
magnetic canopies can act as a global magnetic-arch splicing layer, and find
that the reflections of the solar p-mode oscillations at this magnetic-arch
splicing layer results in significant improvement on the discrepancy between
the observed and calculated p-mode frequencies. The location of the
magnetic-arch splicing layer is determined at a height of about 630\,km, and
the inferred strength of the magnetic field is about 90\,G. These features of
the magnetic-arch splicing layer derived independently in the present study are
quantitatively in agreement with the presence of small-scale magnetic canopies
as those obtained by the observations and 3-D MHD simulations.
