  Young stars interact with their accretion disk through their strong
magnetosphere. We investigate the magnetospheric accretion process in the young
stellar system DoAr 44. We monitored the system over several rotational cycles,
combining high-resolution optical and near-IR spectropolarimetry with
long-baseline near-IR interferometry and multicolor photometry. DoAr 44 is a
young 1.2 solar mass star, moderately accreting from its disk, and seen at a
low inclination. We derive a rotational period of 2.96 d from the system's
light curve. Several optical and near-IR line profiles probing the accretion
funnel flows and the accretion shock are modulated at the stellar rotation
period. The most variable line profile, HeI 1083 nm, exhibits modulated
redshifted wings a signature of accretion funnel flows, as well as deep
blueshifted absorptions indicative of transient outflows. The Zeeman-Doppler
analysis suggests the star hosts a mainly dipolar magnetic field, inclined by
about 20 deg. onto the spin axis, with an intensity reaching about 800 G at the
photosphere, and up to 2 +/- 0.8 kG close to the accretion shock. The magnetic
field appears strong enough to disrupt the inner disk close to the corotation
radius, at a distance of about 4.6 stellar radii (0.043 au). This supports the
upper limit of 5 stellar radii (0.047 au) we derived for the size of the
magnetosphere from long baseline interferometry. DoAr 44 is a pre-transitional
disk system, exhibiting a 25-30 au gap in its circumstellar disk, with the
inner and outer disks being misaligned. On a scale of 0.1 au or less, our
results indicate that the system steadily accretes from its inner disk through
its tilted dipolar magnetosphere. We conclude that in spite of a highly
structured outer disk, perhaps the signature of ongoing planetary formation,
the magnetospheric accretion process proceeds unimpeded at the star-disk
interaction level.
