  Galactic halos accrete material from the intergalactic medium (IGM) and part
of this accretion is expected to be in the form of cool ($T\sim10^4$ K) gas. A
signature of this process could reside in the detection of numerous clouds in
the circumgalactic medium (CGM). However, whether this material is able to
accrete onto the galaxies and feed their star formation or, instead, evaporates
into the CGM hot phase (corona, $T\sim10^6$ K), is not yet understood. Here, we
investigate the evolution of cool CGM clouds accreted from the IGM and falling
through the hot corona of low-redshift disc galaxies, using 3D high-resolution
hydrodynamical simulations. We include the effects of gravity due to the dark
matter halo, isotropic thermal conduction, radiative cooling and an ionizing UV
background. We explored different values of parameters such as the halo mass,
coronal mass, initial cloud velocity and strength of the thermal conduction. We
find that the clouds lose the vast majority of their mass at distances larger
than half of the galaxy virial radius and are completely dissolved in the
corona before reaching the central galaxy. Resolving the Field length with at
least 5-7 cells is crucial to correctly capture the evolution of the infalling
cool gas. Our results indicate that cool IGM accretion can not feed star
formation in $z\sim0$ star-forming galaxies in halos with masses of $10^{11.9}\
M_{\odot}$ or above. This suggests that present-day massive star-forming
galaxies can sustain their star formation only via the spontaneous or induced
cooling of their hot corona.
