Resolving the gap and AU-scale asymmetries in pre-transitional disks of V1247 ORIONIS
Kraus, Stefan; Ireland, M; Sitko, ML; et al.Monnier, John D.; Calvet, Nuria; Espaillat, C; Grady, C; Harries, Tim J.; Hoenig, S; Russell, R; Kim, D; Swearingen, J; Werren, C; Wilner, D
Date: 1 May 2013
Journal
The Astrophysical Journal
Publisher
American Astronomical Society
Publisher DOI
Abstract
Pre-transitional disks are protoplanetary disks with a gapped disk structure, potentially indicating the presence of
young planets in these systems. In order to explore the structure of these objects and their gap-opening mechanism,
we observed the pre-transitional disk V1247 Orionis using the Very Large Telescope Interferometer, the ...
Pre-transitional disks are protoplanetary disks with a gapped disk structure, potentially indicating the presence of
young planets in these systems. In order to explore the structure of these objects and their gap-opening mechanism,
we observed the pre-transitional disk V1247 Orionis using the Very Large Telescope Interferometer, the Keck
Interferometer, Keck-II, Gemini South, and IRTF. This allows us to spatially resolve the AU-scale disk structure
from near- to mid-infrared wavelengths (1.5–13µm), tracing material at different temperatures and over a wide
range of stellocentric radii. Our observations reveal a narrow, optically thick inner-disk component (located at
0.18 AU from the star) that is separated from the optically thick outer disk (radii !46 AU), providing unambiguous
evidence for the existence of a gap in this pre-transitional disk. Surprisingly, we find that the gap region is filled
with significant amounts of optically thin material with a carbon-dominated dust mineralogy. The presence of this
optically thin gap material cannot be deduced solely from the spectral energy distribution, yet it is the dominant
contributor at mid-infrared wavelengths. Furthermore, using Keck/NIRC2 aperture masking observations in the
H, K′
, and L′ bands, we detect asymmetries in the brightness distribution on scales of ∼15–40 AU, i.e., within
the gap region. The detected asymmetries are highly significant, yet their amplitude and direction changes with
wavelength, which is not consistent with a companion interpretation but indicates an inhomogeneous distribution
of the gap material. We interpret this as strong evidence for the presence of complex density structures, possibly
reflecting the dynamical interaction of the disk material with sub-stellar mass bodies that are responsible for the
gap clearing.
Physics and Astronomy
Faculty of Environment, Science and Economy
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