The Disk Substructures at High Angular Resolution Program (DSHARP). VIII. The Rich Ringed Substructures in the AS 209 Disk
Year: 2018
Type: article
Abstract: We present a detailed analysis of the high angular resolution (0.″037, corresponding to 5 au) observations of the 1.25 mm continuum and 12CO 2 − 1 emission from the disk around the T Tauri star AS 209. AS 209 hosts one of the most unusual disks from the Disk Substructures at High Angular Resolution Project sample, the first high angular resolution Atacama Large Millimeter Array survey of disks, as nearly all of the emission can be explained with concentric Gaussian rings. In particular, the dust emission consists of a series of narrow and closely spaced rings in the inner ∼60 au, two well-separated bright rings in the outer disk, centered at 74 and 120 au, and at least two fainter emission features at 90 and 130 au. We model the visibilities with a parametric representation of the radial surface brightness profile, consisting of a central core and seven concentric Gaussian rings. Recent hydrodynamical simulations of low-viscosity disks show that super-Earth planets can produce the multiple gaps seen in AS 209 millimeter continuum emission. The 12CO line emission is centrally peaked and extends out to ∼300 au, much farther than the millimeter dust emission. We find axisymmetric, localized deficits of CO emission around four distinct radii, near 45, 75, 120, and 210 au. The outermost gap is located well beyond the edge of the millimeter dust emission, and therefore cannot be due to dust opacity and must be caused by a genuine CO surface density reduction, due either to chemical effects or depletion of the overall gas content.
Authors: Viviana V. Guzmán, Jane Huang, Sean M. Andrews, Andrea Isella, Laura M. Pérez, John M. Carpenter, Cornelis P. Dullemond, Luca Ricci, Tilman Birnstiel, Shangjia Zhang, Zhaohuan Zhu, Xue-Ning Bai, Myriam Benisty, Karin I. Öberg, David J. Wilner
Institutions: Pontificia Universidad Católica de Chile, Atacama Large Millimeter Submillimeter Array, Center for Astrophysics Harvard & Smithsonian, Rice University, University of Chile, Heidelberg University, California State University, Northridge, Ludwig-Maximilians-Universität München, University of Nevada, Las Vegas, Tsinghua University, Centre National de la Recherche Scientifique, Institut de Planétologie et d'Astrophysique de Grenoble, Université Grenoble Alpes
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
Funders: National Science Foundation, National Aeronautics and Space Administration, National Radio Astronomy Observatory, Deutsche Forschungsgemeinschaft, Agence Nationale de la Recherche, National Science Council, Korea Astronomy and Space Science Institute, National Astronomical Observatory of Japan, Comisión Nacional de Investigación Científica y Tecnológica, Facultad de Ciencias Físicas y Matemáticas, National Institutes of Natural Sciences, H2020 European Research Council
Awards: G113837208, Dusting for the Fingerprints of Planet Formation, G2452576056, G4166165122, RECENT HIGH ANGULAR RESOLUTION OBSERVATIONS (E.G. ALMA VLT) OF PROTOPLANETARY DISKS HAVE BEGUN TO REVEAL COMPLICATED STRUCTURE (E.G. SPIRAL ARMS GAPS RINGS ETC.). IN PRINCIPLE SUCH OBSERVATIONS CAN PROVIDE CONSTRAINTS ON DISK DYNAMICS AND FOR THE FIRST TIME REVEAL THE PHYSICAL PROCESSES WHICH CONTROL THE PLANET FORMATION PROCESS. HOWEVER THIS REQUIRES REALISTIC THEORETICAL MODELS OF DISK DYNAMICS INCLUDING A PROPER TREATMENT OF MHD EFFECTS DUST GROWTH SETTLING AND FEEDBACK AS WELL AS ACCURATE RADIATIVE TRANSFER CALCULATIONS THAT CAN GENERATE SYNTHETIC IMAGES FOR COMPARISON TO DATA. THE GOAL OF THIS PROJECT IS TO COMPUTE SUCH MODELS. WE WILL CALCULATE THE MOST REALISTIC GLOBAL NUMERICAL MODELS OF PROTOPLANETARY DISKS AND DISK-PLANET INTERACTION TO DATE COMPUTE SYNTHETIC IMAGES OF THE MODELS BASED ON A SELF-CONSISTENT TREATMENT OF THE DUST DYNAMICS IN THE DISK AND COMPARE THESE MODELS TO INTERPRET EXISTING DATA AND TO PREDICT FUTURE OBSERVATIONS. IN PARTICULAR WE WILL COMPARE OUR MODELS WITH OBSERVATIONS FROM EXISTING NASA SPACE MISSIONS (E.G. SPITZER HERSCHEL) AND GROUND BASED TELESCOPES (E.G. ALMA EVLA VLT SUBARU GEMINI) AND WE WILL MAKE PREDICTIONS FOR FUTURE OBSERVATIONS. OVER YEARS OUR TEAM HAS BEEN BUILDING TOOLS TO ACHIEVE SUCH GOALS. WE HAVE STUDIED NON-IDEAL MHD EFFECTS ON DISK TURBULENCE DUST PARTICLE DYNAMICS IN GASEOUS DISKS PLANET-DISK INTERACTION AND OTHER ASTROPHYSICAL DISK RELATED PROBLEMS. NOW ADOPTING NOVEL NUMERICAL TECHNIQUES IN OUR NEWLY DEVELOPED 3-D MAGNETOHYDRODYNAMIC (MHD) CODE ATHENA++ WE CAN FINALLY PUT ALL THESE PIECES TOGETHER AND CONSTRUCT FIRST-PRINCIPLE GLOBAL SIMULATIONS TO BE DIRECTLY COMPARED WITH OBSERVATIONS. WE PLAN TO USE THIS NEW CODE TO (1) STUDY HOW PROTOPLANETARY DISKS ACCRETE BY CARRYING OUT GLOBAL 3-D MHD SIMULATIONS INCLUDING ALL IMPORTANT NON-IDEAL MHD EFFECTS. (2) INCLUDE DUST PARTICLES AND YOUNG PLANETS IN OUR SIMULATIONS TO STUDY DUST DYNAMICS PLANETESIMAL FORMATION AND THE OBSERVATIONAL SIGNATURES OF YOUNG PLANETS IN PROTOPLANETARY DISKS. SINCE MOST DISK EMISSION COMES FROM DUST THIS STEP IS ESSENTIAL FOR CONNECTING SIMULATIONS WITH OBSERVATIONS. (3) POST PROCESS OUR GLOBAL 3-D SIMULATIONS WITH 3-D MONTE CARLO RADIATIVE TRANSFER CODES TO GENERATE OBSERVATIONAL SIGNATURES OF DISK TURBULENCE AND YOUNG PLANETS IN DISKS. COMPARISONS WITH CURRENT OBSERVATIONS AND PREDICTIONS FOR FUTURE OBSERVATIONS WILL BE MADE. THESE FIRST-PRINCIPLE CALCULATIONS (INCLUDING MHD EFFECTS DUST-GAS DYNAMICS AND RADIATIVE TRANSFER) WILL ADDRESS FUNDAMENTAL QUESTIONS ON PROTOPLANETARY DISKS AND ALLOW US TO STUDY PLANET FORMATION PROCESSES IN DETAIL. THE PREDICTIONS FROM THESE SIMULATIONS WILL NOT ONLY BE COMPARED WITH OBSERVATIONS (E.G. ALMA) DIRECTLY BUT ALSO SERVE AS A FOUNDATION FOR UNDERSTANDING PLANET FORMATION AND EXOPLANET PROPERTIES FOR FUTURE SPACE MISSIONS (E.G. JWST WFIRST TESS)., G5420063140, Transformational models for Transformational Data, Graduate Research Fellowship Program (GRFP)
OpenAlex ID: W2905116786