THE STRUCTURE OF THE EVOLVED CIRCUMBINARY DISK AROUND V4046 Sgr

2013/08/20 by Katherine A. Rosenfeld, Katherine Rosenfeld, Sean M. Andrews +4 · 7 citations
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Circumbinary planet #Galaxy #Isotopologue #Mass ratio #Molecular Spectroscopy and Structure #Optics #Photoevaporation #Physics #Planet #Population #Protoplanetary disk #Radiative transfer #Spectral energy distribution #Spectral line #Stellar, planetary, and galactic studies #astro-ph.SR

paper · pdf · doi:10.1088/0004-637x/775/2/136

31 pages, 8 figures, accepted for publication in ApJ

arxiv created 2013/08/20 · openalex publication_date 2013/09/16 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

We present sensitive, sub-arcsecond resolution Submillimeter Array observations of the protoplanetary disk around the nearby, pre-main sequence spectroscopic binary V4046 Sgr. We report for the first time a large inner hole ( r = 29 AU) spatially resolved in the 1.3 mm continuum emission and study the structure of this disk using radiative transfer calculations to model the spectral energy distribution, continuum visibilities, and spectral line emission of CO and its main isotopologues. Our modeling scheme demonstrates that the majority of the dust mass is distributed in a narrow ring (centered at 37 AU with a FWHM of 16 AU) that is ∼5 × more compact than the gas disk. This structure implies that the dust-to-gas mass ratio has a strong spatial variation, ranging from a value much larger than typical of the interstellar medium (ISM) at the ring to much smaller than that of the ISM at larger disk radii. We suggest that these basic structural features are potentially observational signatures of the accumulation of solids at a local gas pressure maximum. These models also require a substantial population of ∼μm sized grains inside the central disk cavity. We suggest that this structure is likely the result of dynamical interactions with a low-mass companion, although photoevaporation may also play a secondary role.

Citations

• Evidence for a Developing Gap in a 10 Myr Old Protoplanetary Disk
• A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties
• The Submillimeter Array
• Flows of gas through a protoplanetary gap
• Accretion Disks around Young Objects. III. Grain Growth
• THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES
• X-ray accretion signatures in the close CTTS binary V4046 Sagittarii
• IMAGING THE MOLECULAR DISK ORBITING THE TWIN YOUNG SUNS OF V4046 Sgr
• Dust dynamics during protoplanetary disc clearing
• The Two Micron All Sky Survey (2MASS)
• Dust filtration at gap edges: implications for the spectral energy distributions of discs with embedded planets

Cited by

• Ortho–Para Chemistry of H 2 CO in the Protoplanetary Disk TW Hya
• SCATTERED LIGHT FROM DUST IN THE CAVITY OF THE V4046 Sgr TRANSITION DISK
• LONG-TERM EVOLUTION OF PLANET-INDUCED VORTICES IN PROTOPLANETARY DISKS
• Sulfur Chemistry in Protoplanetary Disks: CS and H2CS
• Chemical enrichment of the planet-forming region as probed by accretion
• The Role of C/O in Nitrile Astrochemistry in PDRs and Planet-forming Disks
• The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines