  SU Aurigae is a widely studied T Tauri star and here we present original
state-of-the-art interferometric observations with better uv and baseline
coverage than previous studies. We aim to investigate the characteristics of
the circumstellar material around SU Aur, constrain the disk geometry,
composition and inner dust rim structure. The MIRC-X instrument at CHARA is a 6
telescope optical beam combiner offering baselines up to 331 m. We undertook
image reconstruction for model-independent analysis, and fitted geometric
models such as Gaussian and ring distributions. Additionally, the fitting of
radiative transfer models constrains the physical parameters of the disk. Image
reconstruction reveals a highly inclined disk with a slight asymmetry
consistent with inclination effects obscuring the inner disk rim through
absorption of incident star light on the near-side and thermal
re-emission/scattering of the far-side. Geometric models find that the
underlying brightness distribution is best modelled as a Gaussian with a FWHM
of $1.53\pm0.01 \mathrm{mas}$ at an inclination of $56.9\pm0.4^\circ$ and minor
axis position angle of $55.9\pm0.5^\circ$. Radiative transfer modelling shows a
flared disk with an inner radius at 0.16 au which implies a grain size of $0.14
\mathrm{\mu m}$ assuming astronomical silicates and a scale height of 9.0 au at
100 au. In agreement with literature, only the dusty disk wind successfully
accounts for the NIR excess by introducing dust above the mid-plane. Our
results confirm and provide better constraints than previous inner disk studies
of SU Aurigae. We confirm the presence of a dusty disk wind in the cicumstellar
environment, the strength of which is enhanced by a late infall event which
also causes very strong misalignments between the inner and outer disks.
