dc.contributor.author | Davies, CL | |
dc.contributor.author | Kraus, S | |
dc.contributor.author | Harries, TJ | |
dc.contributor.author | Kreplin, A | |
dc.contributor.author | Monnier, JD | |
dc.contributor.author | Labdon, A | |
dc.contributor.author | Kloppenborg, B | |
dc.contributor.author | Acreman, DM | |
dc.contributor.author | Baron, F | |
dc.contributor.author | Millan-Gabet, R | |
dc.contributor.author | Sturmann, J | |
dc.contributor.author | Sturmann, L | |
dc.contributor.author | Brummelaar, TAT | |
dc.date.accessioned | 2018-09-05T13:14:09Z | |
dc.date.issued | 2018-10-05 | |
dc.description.abstract | We present comprehensive models of Herbig Ae star, HD 142666, which aim to simultaneously explain its spectral energy distribution (SED) and near-infrared (NIR) interferometry. Our new sub-milliarcsecond resolution CHARA (CLASSIC and CLIMB) interferometric observations, supplemented with archival shorter baseline data from VLTI/PIONIER and the Keck Interferometer, are modeled using centro-symmetric geometric models and an axisymmetric radiative transfer code. CHARA's 330 m baselines enable us to place strong constraints on the viewing geometry, revealing a disk inclined at 58 degrees from face-on with a 160 degree major axis position angle. Disk models imposing vertical hydrostatic equilibrium provide poor fits to the SED. Models accounting for disk scale height inflation, possibly induced by turbulence associated with magneto-rotational instabilities, and invoking grain growth to >1 micron size in the disk rim are required to simultaneously reproduce the SED and measured visibility profile. However, visibility residuals for our best model fits to the SED indicate the presence of unexplained NIR emission, particularly along the apparent disk minor axis, while closure phase residuals indicate a more centro-symmetric emitting region. In addition, our inferred 58 degree disk inclination is inconsistent with a disk-based origin for the UX Ori-type variability exhibited by HD 142666. Additional complexity, unaccounted for in our models, is clearly present in the NIR-emitting region. We propose the disk is likely inclined toward a more edge-on orientation and/or an optically thick outflow component also contributes to the NIR circumstellar flux. | en_GB |
dc.description.sponsorship | C.L.D., S.K., A.K. and A.L. acknowledge support
from the ERC Starting Grant \ImagePlanetFormDiscs"
(Grant Agreement No. 639889), STFC Rutherford
fellowship/grant (ST/J004030/1, ST/K003445/1) and
Philip Leverhulme Prize (PLP-2013-110). J.D.M., F.B.,
and B.K. acknowledge support from NSF grants AST-
1210972 and AST-1506540. We would like to thank
Bernard Lazareff, Jean-Baptiste Le Bouquin and Rachel
Akeson for their assistance in acquiring archival data
for HD142666. This work is based upon observations
obtained with the Georgia State University Center for
High Angular Resolution Astronomy Array at Mount
Wilson Observatory. The CHARA Array is supported
by the National Science Foundation under Grant No.
AST-1211929. Institutional support has been provided
from the GSU College of Arts and Sciences and the GSU
Office of the Vice President for Research and Economic
Development. The calculations for this paper were performed
on the University of Exeter Supercomputer, a
DiRAC Facility jointly funded by STFC, the Large Facilities
Capital Fund of BIS, and the University of Exeter. | en_GB |
dc.identifier.citation | Vol. 866 (1), article 23 | en_GB |
dc.identifier.doi | 10.3847/1538-4357/aade51 | |
dc.identifier.uri | http://hdl.handle.net/10871/33917 | |
dc.language.iso | en | en_GB |
dc.publisher | American Astronomical Society / IOP Publishing | en_GB |
dc.rights | © 2018. The American Astronomical Society. All rights reserved | |
dc.subject | infrared: stars | en_GB |
dc.subject | protoplanetary disks | en_GB |
dc.subject | stars: formation | en_GB |
dc.subject | stars: individual: HD142666 | en_GB |
dc.subject | stars: variables: Herbig Ae/Be | en_GB |
dc.subject | techniques: interferometric | en_GB |
dc.title | Simultaneous spectral energy distribution and near-infrared interferometry modeling of HD 142666 | en_GB |
dc.type | Article | en_GB |
dc.description | This is the final version. Available from American Astronomical Society via the DOI in this record | en_GB |
dc.identifier.journal | Astrophysical Journal | en_GB |