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Title: Modeling Dust Emission of HL Tau Disk Based on Planet-Disk Interactions

Abstract

In this paper, 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 Jup at 13.1, 33.0, and 68.6 AU, respectively. Finally, implications for the planet formation as well as the limitations of this scenario are discussed.

Authors:
 [1];  [2];  [3];  [2];  [4]
  1. Chinese Academy of Sciences (CAS), Nanjing (China). Purple Mountain Observatory. Key Lab. of Planetary Sciences; Los Alamos National Lab. (LANL), Los Alamos, NM (United States). Theoretical Division
  2. Los Alamos National Lab. (LANL), Los Alamos, NM (United States). Theoretical Division
  3. Rice Univ., Houston, TX (United States)
  4. Chinese Academy of Sciences (CAS), Nanjing (China). Purple Mountain Observatory. Key Lab. of Planetary Sciences
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Chinese Academy of Sciences (CAS), Nanjing (China)
Sponsoring Org.:
USDOE Laboratory Directed Research and Development (LDRD) Program; National Science Foundation (NSF); National Aeronautic and Space Administration (NASA); National Natural Science Foundation of China (NNSFC); Chinese Academy of Sciences; Natural Science Foundation of Jiangsu Province (China)
Contributing Org.:
Rice Univ., Houston, TX (United States)
OSTI Identifier:
1335605
Report Number(s):
LA-UR-15-28170
Journal ID: ISSN 1538-4357
Grant/Contract Number:  
AC52-06NA25396; 1535809; NNX15AB06G; 11273068; 11473073; 11503092; XDB09000000; KJZD-EW-Z001; BK20141509
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 818; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; astronomy and astrophysics; planet–disk interactions; protoplanetary disks; submillimeter: planetary systems; techniques: interferometric

Citation Formats

Jin, Sheng, Li, Shengtai, Isella, Andrea, Li, Hui, and Ji, Jianghui. Modeling Dust Emission of HL Tau Disk Based on Planet-Disk Interactions. United States: N. p., 2016. Web. doi:10.3847/0004-637X/818/1/76.
Jin, Sheng, Li, Shengtai, Isella, Andrea, Li, Hui, & Ji, Jianghui. Modeling Dust Emission of HL Tau Disk Based on Planet-Disk Interactions. United States. doi:10.3847/0004-637X/818/1/76.
Jin, Sheng, Li, Shengtai, Isella, Andrea, Li, Hui, and Ji, Jianghui. Tue . "Modeling Dust Emission of HL Tau Disk Based on Planet-Disk Interactions". United States. doi:10.3847/0004-637X/818/1/76. https://www.osti.gov/servlets/purl/1335605.
@article{osti_1335605,
title = {Modeling Dust Emission of HL Tau Disk Based on Planet-Disk Interactions},
author = {Jin, Sheng and Li, Shengtai and Isella, Andrea and Li, Hui and Ji, Jianghui},
abstractNote = {In this paper, 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 MJup at 13.1, 33.0, and 68.6 AU, respectively. Finally, implications for the planet formation as well as the limitations of this scenario are discussed.},
doi = {10.3847/0004-637X/818/1/76},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 818,
place = {United States},
year = {2016},
month = {2}
}

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