  We present an optical/near-IR survey of 11 variable young stars (EXors and
EXor candidates) aimed at deriving and monitoring their accretion properties.
About 30 optical and near-infrared spectra ($\Re$ $\sim$ 1500-2000) were
collected between 2014-2019 with the Large Binocular Telescope (LBT). From the
spectral analysis we have derived the accretion luminosity and mass accretion
rate, the visual extinction, the temperature and density of the permitted line
formation region, and the signature of the outflowing matter.
  Two sources (ASASSN-13db and iPTF15afq) have been observed in outburst and
quiescence, three during a high-level of brightness (XZ Tau, PV Cep, and NY
Ori), and the others in quiescence. These latter have accretion luminosity and
mass accretion rates in line with the values measured in classical T Tauri
stars of similar mass. All sources observed more than once present accretion
variability. The most extreme case is ASASSN-13db, for which the mass accretion
rate decreases by two orders of magnitude from the outburst peak in 2015 to
quiescence in 2017. Also, in NY Ori the accretion luminosity decreases by a
factor 25 in one year. In 80% of the sample we detect the [OI]630 nm line, a
tracer of mass loss. From the variability of the H$\alpha$/[OI]630, ratio, we
conclude that mass accretion variations are larger than mass loss variations.
From the analysis of the HI recombination lines a correlation is suggested
between the density of the line formation region and the level of accretion
activity of the source.
