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

Nathanial P. Hendler, Paola Pinilla, Ilaria Pascucci, Adriana Pohl, Gijs Mulders, Thomas Henning, Ruobing Dong, Cathie Clarke, James Owen, David Hollenbach

Research output: Contribution to journalArticlepeer-review

Abstract

We present high resolution (0.1100 × 0.0600) 3 mm ALMA observations of the highly inclined transition disk around the star T Cha. Our continuum image reveals multiple dust structures: an inner disk, 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 18-28 au, and the emission from the outer ring peaks at ∼ 36 au. We compare our ALMA image with previously published 1.6µm 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 disk are located further 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-disk 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.

Original languageEnglish (US)
JournalUnknown Journal
StatePublished - Nov 27 2017

Keywords

  • Circumstellar matter
  • Planet
  • Planet-disk interactions
  • Planets and satellites: detection
  • Protoplanetary disks
  • Satellites: formation

ASJC Scopus subject areas

  • General

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