  The Galactic disk is one of the main components of the Milky Way, which
contributes most of the luminosity. Its structure is essential for
understanding the formation and evolution of the Milky Way. Using 174,443
K-type dwarf stars observed by both LAMOST and Gaia DR3, we study the disk
density profile in the local volume within 1,200 pc. In the azimuthal
dimension, we find strong asymmetric signal of the thin disk. The surface
density and the scale height of the southern disk significantly change versus
the azimuthal angle at the same galactocentric distance $R$. Meanwhile, in the
vertical dimension, the scale height of the northern disk has quite different
trend than that of the southern one. The scale height of the southern disk
shows a decreasing trend with $\phi\sim-2.5^\circ$, and change to an increasing
one with $\phi\sim5.0^\deg$. Meanwhile, the scale height of the northern disk
has a consistently smaller increase. Finally, we divide the entire sample into
three subsamples based on metallicity and all three subsamples show significant
non-axisymmetric and north-south asymmetric signals in the Galactic disk.
Furthermore, we find that the scale height of the metal-poor ([Fe/H] $<$ -0.4
dex) subsample in the northern disk is greater than that of the metal-rich
([Fe/H] $>$ -0.1 dex) subsample. However, in the southern disk, the scale
height exhibits varying relationships across different metallicity slices.
