Dusty disk winds at the sublimation rim of the highly inclined, low mass YSO SU Aurigae. (arXiv:1905.11907v1 [astro-ph.EP])

Dusty disk winds at the sublimation rim of the highly inclined, low mass YSO SU Aurigae. (arXiv:1905.11907v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Labdon_A/0/1/0/all/0/1">Aaron Labdon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_S/0/1/0/all/0/1">Stefan Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_C/0/1/0/all/0/1">Claire L Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreplin_A/0/1/0/all/0/1">Alexander Kreplin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kluska_J/0/1/0/all/0/1">Jacques Kluska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harries_T/0/1/0/all/0/1">Tim J Harries</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monnier_J/0/1/0/all/0/1">John D Monnier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brummelaar_T/0/1/0/all/0/1">Theo ten Brummelaar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baron_F/0/1/0/all/0/1">Fabian Baron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millan_Gabet_R/0/1/0/all/0/1">Rafael Millan-Gabet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kloppenborg_B/0/1/0/all/0/1">Brian Kloppenborg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eisner_J/0/1/0/all/0/1">Joshua Eisner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sturmann_J/0/1/0/all/0/1">Judit Sturmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sturmann_L/0/1/0/all/0/1">Laszlo Sturmann</a>

T Tauri stars are low-mass young stars whose disks provide the setting for
planet formation. Despite this, their structure is poorly understood. We
present new infrared interferometric observations of the SU Aurigae
circumstellar environment that offer 3 x higher resolution and better baseline
position angle coverage over previous observations. We investigate the
characteristics of circumstellar material around SU Aur, constrain the disk
geometry, composition and inner dust rim structure. The CHARA array offers
opportunities for long baseline observations, with baselines up to 331 m. Using
the CLIMB 3-telescope combiner in the K-band allows us to measure visibilities
as well as closure phase. We undertook image reconstruction for
model-independent analysis, and geometric modeling. Additionally, the fitting
of radiative transfer models constrains the physical parameters of the disk.
For the first time, a dusty disk wind is introduced to the radiative transfer
code TORUS to model protoplanetary disks. Our implementation is motivated by
theoretical dusty disk winds, where magnetic field lines drive dust above the
disk plane close to the sublimation zone. Image reconstruction reveals an
inclined disk with slight asymmetry along its minor-axis, likely due to
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 modelling of a skewed ring finds the inner rim at 0.17+/-0.02 au with
an inclination of 50.9+/-1.0 degrees and minor axis position angle 60.8+/-1.2
degrees. Radiative transfer modelling shows a flared disk with an inner radius
at 0.18 au which implies a grain size of 0.4 um and a scale height of 15.0 au
at 100 au. Among the tested radiative transfer models, only the dusty disk wind
successfully accounts for the K-band excess by introducing dust above the
mid-plane.

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