SU-Aur MIRCX interferometric observations

Additionally, the fitting of radiative transfer models constrained 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 Full-Width Half-Maximum (FWHM) of 1.53+/-0.01mas at an inclination of 56.9+/-0.4{deg} and a minor axis position angle of 55.9+/-0.5{deg}.

Radiative transfer modelling shows a flared disk with an inner radius at 0.16au which implies a grain size of 0.14um assuming astronomical silicates and a scale height of 9.0au at 100au. In agreement with the literature, only the dusty disk wind successfully accounts for the near infrared (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 circumstellar environment, the strength of which is enhanced by a late infall event which also causes very strong misalignments between the inner and outer disks.