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(Abridged) By means of high-resolution cosmological simulations in thecontext of the LCDM scenario, the specific star formation rate (SSFR=SFR/Ms, Msis the stellar mass)--Ms and stellar mass fraction (Fs=Ms/Mh, Mh is the halomass)--Ms relations of low-mass galaxies (2.5< Mh/10^10 Msun <50 at redshiftz=0) at different epochs are predicted. The Hydrodynamics ART code was used andsome variations of the sub-grid parameters were explored. Most of simulatedgalaxies, specially those with the highest resolutions, have significant diskcomponents and their structural and dynamical properties are in reasonableagreement with observations of sub-M* field galaxies. However, the SSFRs are5-10 times smaller than the averages of several (compiled and homogenized here)observational determinations for field blue/star-forming galaxies at z<0.3 (atlow masses, most of observed field galaxies are actually blue/star-forming).This inconsistency seems to remain even at z~1.5 though less drastic. The Fs ofsimulated galaxies increases with Mh as semi-empirical inferences show, but inabsolute values the former are ~5-10 times larger than the latter at z=0; thisdifference increases probably to larger factors at z~1-1.5. The inconsistenciesreported here imply that simulated low-mass galaxies (0.2<Ms/10^9 Msun <30 atz=0) assembled their stellar masses much earlier than observations suggest.This confirms the predictions previously found by means of LCDM-based models ofdisk galaxy formation and evolution for isolated low-mass galaxies (Firmani &Avila-Reese 2010), and highlight that our implementation of astrophysics intosimulations and models are still lacking vital ingredients.

The specific star formation rate and stellar mass fraction of low-mass central galaxies in cosmological simulations