  We used the TNG/GIANO instrument to obtain near-IR high-resolution spectra
(R~50000) of XZ Tau and DR Tau, two actively accreting T Tauri stars classified
as EXors. The analysis of the observed features provides information on the
properties of the inner disk, the accretion columns, and the winds. Both
sources display composite HI line profiles, with contributions from both
accreting gas and high-velocity winds. These lines become more symmetric and
narrower with increasing upper energy, which may be interpreted in terms of two
components with different decrements or imputed to self-absorption effects. XZ
Tau shows a relatively high state of activity with respect to literature
observations. The variation of the HeI 1.08um line blue-shifted absorption
suggests that the inner wind has undergone a dramatic change in its velocity
structure, connected with a recent accretion event. DR Tau has a more stable
wind as its HeI 1.08um absorption is stable in time in spite of strong
variability of the emission component. The IR veiling can be interpreted as due
to blackbody emission at temperatures of 1600K for XZ Tau and 2300K DR Tau,
with emitting areas ~30 times larger than the star. For XZ Tau these conditions
are consistent with emission from the inner rim of the dusty disk, while for DR
Tau the fairly high temperature may suggest an origin from a thick gaseous disk
within the dust sublimation radius. Strong and broad metallic lines, mainly
from CI and FeI, are detected in XZ Tau, similar to those observed in other
EXor sources during burst phases. DR Tau shows weaker and narrower metallic
lines, despite its larger accretion luminosity. This suggests that accretion is
not the only driver of metallic line excitation. Our observations show the
potential of wide-band, high-resolution near-IR spectroscopy to simultaneously
probe the phenomena that occur in the star-disk interaction region.
