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Galactic halos accrete material from the intergalactic medium (IGM) and partof this accretion is expected to be in the form of cool ($T\sim10^4$ K) gas. Asignature of this process could reside in the detection of numerous clouds inthe circumgalactic medium (CGM). However, whether this material is able toaccrete onto the galaxies and feed their star formation or, instead, evaporatesinto the CGM hot phase (corona, $T\sim10^6$ K), is not yet understood. Here, weinvestigate the evolution of cool CGM clouds accreted from the IGM and fallingthrough the hot corona of low-redshift disc galaxies, using 3D high-resolutionhydrodynamical simulations. We include the effects of gravity due to the darkmatter halo, isotropic thermal conduction, radiative cooling and an ionizing UVbackground. We explored different values of parameters such as the halo mass,coronal mass, initial cloud velocity and strength of the thermal conduction. Wefind that the clouds lose the vast majority of their mass at distances largerthan half of the galaxy virial radius and are completely dissolved in thecorona before reaching the central galaxy. Resolving the Field length with atleast 5-7 cells is crucial to correctly capture the evolution of the infallingcool gas. Our results indicate that cool IGM accretion can not feed starformation 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-forminggalaxies can sustain their star formation only via the spontaneous or inducedcooling of their hot corona.

Clouds accreting from the IGM are not able to feed the star formation of low-redshift disc galaxies