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We investigate the chemical and kinematic properties of the diffuse stellarhaloes of six simulated Milky Way-like galaxies from the Aquarius Project.Binding energy criteria are adopted to defined two dynamically distinct stellarpopulations: the diffuse inner and outer haloes, which comprise differentstellar sub-populations with particular chemical and kinematic characteristics.Our simulated inner- and outer-halo stellar populations have receivedcontributions from debris stars (formed in sub-galactic systems while they wereoutside the virial radius of the main progenitor galaxies) and endo-debrisstars (those formed in gas-rich sub-galactic systems inside the dark matterhaloes). The inner haloes possess an additional contribution from disc-heatedstars in the range $\sim 3 - 30 %$, with a mean of $\sim 20% $. Disc-heatedstars might exhibit signatures of kinematical support, in particular among theyoungest ones. Endo-debris plus disc-heated stars define the so-called \insitustellar populations. In both the inner- and outer-halo stellar populations, wedetect contributions from stars with moderate to low [$\alpha$/Fe] ratios,mainly associated with the endo-debris or disc-heated sub-populations. Theobserved abundance gradients in the inner-halo regions are influenced by boththe level of chemical enrichment and the relative contributions from eachstellar sub-population. Steeper abundance gradients in the inner-halo regionsare related to contributions from the disc-heated and endo-debris stars, whichtend to be found at lower binding energies than debris stars. (Abridged).

Stellar haloes of simulated Milky Way-like galaxies: Chemical and kinematic properties