  Low-mass X-ray binaries (LMXBs) are systems in which a low-mass companion
transfers mass via Roche-lobe overflow onto a black hole (BH) or a weakly
magnetized neutron star (NS). It is believed that both the solid surface and
the magnetic field of an NS can affect the accretion flow and show some
observable effects. Using the disk emission dominant data, we compare the disk
evolution of the two types of systems from low luminosity to super-Eddington
luminosity. As the luminosity decreases the disk in the NS LMXB 4U1608--522
begins to leave the innermost stable circular orbit (ISCO) at much higher
luminosity ($\sim$ 0.1 $L_{\mathrm{Edd}}$), compared with BH LMXBs at much
lower luminosity ($\sim$ 0.03 $L_{\mathrm{Edd}}$), due to the interaction
between the NS magnetosphere and accretion flow. However, as the luminosity
increases above a critical luminosity, the disks in BH and NS LMXBs trace the
same evolutionary pattern, because the magnetosphere is restricted inside ISCO,
and then both the NS surface emission and (dipole) magnetic field do not
significantly affect the secular evolution of the accretion disk, that is
driven by the increased radiation pressure in the inner region. We further
suggest that the NS surface emission provides additional information of
accretion disk, not available in BH systems. Through the observed NS surface
emission, we argue that the disk thickness $H/R$ is less than $0.3-0.4$, and
that the significant outflow from inner disk edge exists at luminosity close to
Eddington luminosity.
