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MODELING DUST EMISSION OF HL TAU DISK BASED ON PLANET–DISK INTERACTIONS

Journal Article · · Astrophysical Journal
;  [1]; ;  [2];  [3]
  1. Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China)
  2. Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)
  3. Rice University, Houston, TX (United States)
+ Show Author Affiliations
We use extensive global two-dimensional hydrodynamic disk gas+dust simulations with embedded planets, coupled with three-dimensional radiative transfer calculations, to model the dust ring and gap structures in the HL Tau protoplanetary disk observed with the Atacama Large Millimeter/Submillimeter Array (ALMA). We include the self-gravity of disk gas and dust components and make reasonable choices of disk parameters, assuming an already settled dust distribution and no planet migration. We can obtain quite adequate fits to the observed dust emission using three planets with masses of 0.35, 0.17, and 0.26 M{sub Jup} at 13.1, 33.0, and 68.6 AU, respectively. Implications for the planet formation as well as the limitations of this scenario are discussed.
OSTI ID:
22521571
Journal Information:
Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 818; ISSN ASJOAB; ISSN 0004-637X
Country of Publication:
United States
Language:
English

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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
COMPUTERIZED SIMULATION
COSMIC DUST
GRAVITATION
MASS
PLANETS
PROTOPLANETS
RADIANT HEAT TRANSFER