New Spatially Resolved Imaging of the SR 21 Transition Disk and Constraints on the Small-grain Disk Geometry
Skemer, A. J.
Eisner, J. A.
van der Marel, N.
Sheehan, P. D.
Close, L. M.
Ireland, M. J.
Males, J. M.
Morzinski, K. M.
Bailey, V. P.
AffiliationUniv Arizona, Astron Dept
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationS. Sallum et al 2019 ApJ 883 100
RightsCopyright © 2019. The American Astronomical Society.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractWe present new 0.6-4 mu m imaging of the SR 21 transition disk from Keck/NIRC2 and Magellan/MagAO. The protoplanetary disk around SR 21 has a large (similar to 30-40 au) clearing first inferred from its spectral energy distribution and later detected in submillimeter imaging. Both the gas and small dust grains are known to have a different morphology, with an inner truncation in CO at similar to 7 au, and micron-sized dust detected within the millimeter clearing. Previous near-infrared imaging could not distinguish between an inner dust disk with a truncation at similar to 7 au or one that extended to the sublimation radius. The imaging data presented here require an inner dust disk radius of a few au, and complex structure such as a warp or spiral. We present a parametric warped disk model that can reproduce the observations. Reconciling the images with the spectral energy distribution gathered from the literature suggests grain growth to greater than or similar to 2-5 mu m within the submillimeter clearing. The complex disk structure and possible grain growth can be connected to dynamical shaping by a giant-planet-mass companion, a scenario supported by previous observational and theoretical studies.
VersionFinal published version
SponsorsNSF Astronomy and Astrophysics Postdoctoral FellowshipNational Science Foundation (NSF) [AST-1701489]; NSFNational Science Foundation (NSF) ; NASA Exoplanets Research Program (XRP) [NNX16AD44G]; W. M. Keck FoundationW.M. Keck Foundation