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A tale of two Herbig Ae stars, MWC 275 and AB Aurigae: comprehensive models for spectral energy distribution and interferometry

Tannirkulam, A. and Monnier, J. D. and Harries, T. J. and Millan-Gabet, R. and Zhu, Z. and Pedretti, L. and Ireland, M. and Tuthill, P. and ten Brummelaar, T. and McAlister, H. and Farrington, C. and Goldfinger, P. J. and Sturmann, J. and Sturmann, L. and Turner, N. (2008) A tale of two Herbig Ae stars, MWC 275 and AB Aurigae: comprehensive models for spectral energy distribution and interferometry. Astrophysical Journal, 689 . pp. 513-531. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20090723-105800458

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Abstract

We present comprehensive models for the Herbig Ae stars MWC 275 and AB Aur that aim to explain their spectral energy distribution (from UV to millimeter) and long-baseline interferometry (from near-infrared to millimeter) simultaneously. Data from the literature, combined with new mid-infrared (MIR) interferometry from the Keck Segment Tilting Experiment, are modeled using an axisymmetric Monte Carlo radiative transfer code. Models in which most of the near-infrared (NIR) emission arises from a dust rim fail to fit the NIR spectral energy distribution (SED) and sub-milliarcsecond NIR CHARA interferometry. Following recent work, we include an additional gas emission component with similar size scale to the dust rim, inside the sublimation radius, to fit the NIR SED and long-baseline NIR interferometry on MWC 275 and AB Aur. In the absence of shielding of starlight by gas, we show that the gas-dust transition region in these YSOs will have to contain highly refractory dust, sublimating at ~1850 K. Despite having nearly identical structure in the thermal NIR, the outer disks of MWC 275 and AB Aur differ substantially. In contrast to the AB Aur disk, MWC 275 lacks small grains in the disk atmosphere capable of producing significant 10-20 μm emission beyond ~7 AU, forcing the outer regions into the "shadow" of the inner disk.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/592346DOIArticle
http://www.iop.org/EJ/abstract/0004-637X/689/1/513PublisherArticle
ORCID:
AuthorORCID
Tannirkulam, A.0000-0002-9396-5551
Monnier, J. D.0000-0002-3380-3307
Harries, T. J.0000-0001-8228-9503
Millan-Gabet, R.0000-0003-0447-5866
Ireland, M.0000-0002-6194-043X
ten Brummelaar, T.0000-0002-0114-7915
Farrington, C.0000-0001-9939-2830
Turner, N.0000-0001-8292-1943
Additional Information:© 2008. The American Astronomical Society. Received 2008 May 19; accepted 2008 August 8. A. T. acknowledges contributions from Nuria Calvet,Michael Busha, Marlin Whitaker, and Steve Golden. Research at the CHARA array is supported by the National Science Foundation through grants AST 06-06958 and AST 03-52723 and by the Georgia State University through the offices of the Dean of the College of Arts and Sciences and the Vice President for Research. This project was partially supported by NASA grant 050283. This publication makes use of NASA’s Astrophysics Data System Abstract Service. CHARA visibility-calibrator sizes were obtained with the fBol module of getCal, a package made available by the Michelson Science Center, California Institute of Technology (http://msc.caltech.edu). Computations were performed on the Legato-Opus Cluster Network at the University of Michigan.
Funders:
Funding AgencyGrant Number
NSFAST 06-06958
NSFAST 03-52723
Georgia State UniversityUNSPECIFIED
NASA050283
Subject Keywords:circumstellar matter, planetary systems: protoplanetary disks, radiative transfer, stars: preYmain, sequence, techniques: interferometric
Record Number:CaltechAUTHORS:20090723-105800458
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20090723-105800458
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:14653
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:10 Aug 2009 16:10
Last Modified:09 Mar 2020 13:19

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