SIMBAD references

We present a multiwavelength study of three star-forming regions, spanning the age range 1-14 Myr, located between the 30 Doradus complex and supernova SN 1987A in the Large Magellanic Cloud (LMC). We reliably identify about 1000 pre-main-sequence (PMS) star candidates actively undergoing mass accretion and estimate their stellar properties and mass accretion rate ({dot}M). Our measurements represent the largest {dot}M data set of low-metallicity stars presented so far. As such, they offer a unique opportunity to study on a statistical basis the mass accretion process in the LMC and, more in general, the evolution of the mass accretion process around low-metallicity stars. We find that the typical {dot}M of PMS stars in the LMC is higher than for galactic PMS stars of the same mass, independently of their age. Taking into account the caveats of isochronal age and {dot}M estimates, the difference in {dot}M between the LMC and our Galaxy appears to be about an order of magnitude. We review the main mechanisms of disc dispersal and find indications that typically higher {dot}M are to be expected in low-metallicity environments. However, many issues of this scenario need to be clarified by future observations and modelling. We also find that, in the mass range 1-2 M_☉,{dot}M of PMS stars in the LMC increases with stellar mass as {dot}M ∝M_*^b, with b ≈ 1, i.e. slower than the second power law found for galactic PMS stars in the same mass regime.