  Young stellar objects are thought to accrete material from their
circumstellar disks through their strong stellar magnetospheres. We aim to
directly probe the magnetospheric accretion region on a scale of a few 0.01 au
in a young stellar system using long-baseline optical interferometry. We
observed the pre-transitional disk system DoAr 44 with VLTI/GRAVITY on two
consecutive nights in the K-band. We computed interferometric visibilities and
phases in the continuum and in the BrG line in order to constrain the extent
and geometry of the emitting regions. We resolve the continuum emission of the
inner dusty disk and measure a half-flux radius of 0.14 au. We derive the
inclination and position angle of the inner disk, which provides direct
evidence that the inner and outer disks are misaligned in this pre-transitional
system. This may account for the shadows previously detected in the outer disk.
We show that BrG emission arises from an even more compact region than the
inner disk, with an upper limit of 0.047 au (5 Rstar). Differential phase
measurements between the BrG line and the continuum allow us to measure the
astrometric displacement of the BrG line-emitting region relative to the
continuum on a scale of a few tens of microarcsec, corresponding to a fraction
of the stellar radius. Our results can be accounted for by a simple geometric
model where the BrG line emission arises from a compact region interior to the
inner disk edge, on a scale of a few stellar radii, fully consistent with the
concept of magnetospheric accretion process in low-mass young stellar systems.
