Modeling the Infrared Emission from the HD 141569A Disk

Abstract

We model the infrared (IR) emission from the double-ring disk of HD 141569A, using a porous dust model that was previously shown successful in reproducing the spectral energy distributions (SEDs) of the disks around $\beta$ Pictoris and HR 4796A. The dust consists of either unaltered or highly processed interstellar materials and vacuum with a volume fraction of ~90%. Together with a population of polycyclic aromatic hydrocarbon (PAH) molecules of which a large fraction is charged, the porous dust model made of coagulated but otherwise unaltered protostellar interstellar grains provides an excellent fit to the entire SED from the mid-IR to millimeter wavelengths including the PAH mid-IR emission features. The nondetection of the 21 micron crystalline silicate feature predicted from the porous dust model composed of highly-processed grains (mainly crystalline silicate dust) imposes an upper limit of ~10% on the mass fraction of crystalline silicates. Spectroscopic and broadband photometric predictions are made for SIRTF observations which will provide further tests of the applicability of the porous dust model to circumstellar disks.

published in The Astrophysical Journal, vol. 594, pp. 987--1010; 46 pages; 12 figures

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• PAH chemistry and IR emission from circumstellar disks
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• Polycyclic aromatic hydrocarbon ionization as a tracer of gas flows through protoplanetary disk gaps
• Structuring the HD 141569 A circumstellar dust disk. Impact of eccentric bound stellar companions
• Modeling the gas-phase chemistry of the transitional disk around HD 141569A
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• Hubble and Spitzer Space Telescope Observations of the Debris Disk around the Nearby K Dwarf HD 92945
• Gas lines from the 5-Myr old optically thin disk around HD141569A. Herschel observations and modeling
• Characterization of the inner disk around HD 141569 A from Keck/NIRC2 L-band vortex coronagraphy
• Probing midplane CO abundance and gas temperature with DCO${}^{+}$ in the protoplanetary disk around HD 169142
• A Dynamical Simulation of the Debris Disk Around HD 141569A
• What can we learn about protoplanetary disks from analysis of mid-infrared carbonaceous dust emission?
• Compact pebbles and the evolution of volatiles in the interstellar comet 2I/Borisov
• Resolved Gas Interior to the Dust Rings of the HD 141569 Disk
• Nano carbon dust emission in proto-planetary disks: the aliphatic-aromatic components
• Modeling the Infrared Emission from the Epsilon Eridani Disk
• Complex Organic Materials in the HR 4796A Disk?
• PAHs in Comets: An Overview
• On the Anomalous Silicate Emission Features of AGNs: A Possible Interpretation Based on Porous Dust
• Spinning dust emission from circumstellar disks and its role in excess microwave emission
• Dust and Polycyclic Aromatic Hydrocarbon in the Pre-Transitional Disk around HD 169142
• Limits on the Optical Brightness of the Epsilon Eridani Dust Ring
• The influence of dust grain porosity on the analysis of debris disc observations
• Dust and Polycyclic Aromatic Hydrocarbon in the HD 34700 Debris Disk
• Evolution of PAHs in protoplanetary disks
• Toward understanding the 3.4 micron and 9.7 micron extinction feature variations from the local diffuse interstellar medium to the Galactic center
• The GRAVITY Young Stellar Object survey VIII. Gas and dust faint inner rings in the hybrid disk of HD141569
• Light Scattering and Thermal Emission by Primitive Dust Particles in Planetary Systems
• Imaging the 44 AU Kuiper Belt-analogue debris ring around HD 141569A with GPI polarimetry
• Restructuring and destruction of hydrocarbon dust in the interstellar medium
• The Mid-Infrared Polarization of the Herbig Ae Star WL 16: An Interstellar Origin?
• Spatially resolving polycyclic aromatic hydrocarbons in Herbig Ae disks with VISIR-NEAR at the VLT