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Journal Article

A likely planet-induced gap in the disc around T Cha

MPS-Authors

Hendler,  Nathanial P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pinilla,  Paola
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pascucci,  Ilaria
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pohl,  Adriana
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mulders,  Gijs
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Henning,  Thomas
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dong,  Ruobing
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Clarke,  Cathie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Owen,  James
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hollenbach,  David
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018MNRAS.475L..62H
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Citation

Hendler, N. P., Pinilla, P., Pascucci, I., Pohl, A., Mulders, G., Henning, T., et al. (2018). A likely planet-induced gap in the disc around T Cha. Monthly Notices of the Royal Astronomical Society, 475, L62-L66.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CD5A-0
Abstract
We present high-resolution (0.11 × 0.06 arcsec2) 3 mm ALMA observations of the highly inclined transition disc around the star T Cha. Our continuum image reveals multiple dust structures: an inner disc, a spatially resolved dust gap, and an outer ring. When fitting sky-brightness models to the real component of the 3 mm visibilities, we infer that the inner emission is compact (≤1 au in radius), the gap width is between 18 and 28 au, and the emission from the outer ring peaks at ̃36 au. We compare our ALMA image with previously published 1.6 μm VLT/SPHERE imagery. This comparison reveals that the location of the outer ring is wavelength dependent. More specifically, the peak emission of the 3 mm ring is at a larger radial distance than that of the 1.6 μm ring, suggesting that millimeter-sized grains in the outer disc are located farther away from the central star than micron-sized grains. We discuss different scenarios to explain our findings, including dead zones, star-driven photoevaporation, and planet-disc interactions. We find that the most likely origin of the dust gap is from an embedded planet, and estimate - for a single planet scenario - that T Cha's gap is carved by a 1.2MJup planet.