New Constraints on Turbulence and Embedded Planet Mass in the HD 163296 Disk from Planet–Disk Hydrodynamic Simulations

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dc.citation.articleNumber87en_US
dc.citation.issueNumber2en_US
dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.volumeNumber857en_US
dc.contributor.authorLiu, Shang-Feien_US
dc.contributor.authorJin, Shengen_US
dc.contributor.authorLi, Shengtaien_US
dc.contributor.authorIsella, Andreaen_US
dc.contributor.authorLi, Huien_US
dc.date.accessioned2018-08-21T16:18:44Zen_US
dc.date.available2018-08-21T16:18:44Zen_US
dc.date.issued2018en_US
dc.description.abstractRecent Atacama Large Millimeter and Submillimeter Array (ALMA) observations of the protoplanetary disk around the Herbig Ae star HD 163296 revealed three depleted dust gaps at 60, 100, and 160 au in the 1.3 mm continuum as well as CO depletion in the middle and outer dust gaps. However, no CO depletion was found in the inner dust gap. To examine the planet–disk interaction model, we present results of 2D two fluid (gas + dust) hydrodynamic simulations coupled with 3D radiative transfer simulations. To fit the high gas-to-dust ratio of the first gap, we find that the Shakura–Sunyaev viscosity parameter α must be very small ($\lesssim {10}^{-4}$) in the inner disk. On the other hand, a relatively large α ($\sim 7.5\times {10}^{-3}$) is required to reproduce the dust surface density in the outer disk. We interpret the variation of α as an indicator of the transition from an inner dead zone to the outer magnetorotational instability (MRI) active zone. Within ~100 au, the HD 163296 disk's ionization level is low, and non-ideal magnetohydrodynamic effects could suppress the MRI, so the disk can be largely laminar. The disk's ionization level gradually increases toward larger radii, and the outermost disk ($r\gt 300$ au) becomes turbulent due to MRI. Under this condition, we find that the observed dust continuum and CO gas line emissions can be reasonably fit by three half-Jovian-mass planets (0.46, 0.46, and $0.58\,{M}_{{\rm{J}}}$) at 59, 105, and 160 au, respectively.en_US
dc.identifier.citationLiu, Shang-Fei, Jin, Sheng, Li, Shengtai, et al.. "New Constraints on Turbulence and Embedded Planet Mass in the HD 163296 Disk from Planet–Disk Hydrodynamic Simulations." <i>The Astrophysical Journal,</i> 857, no. 2 (2018) IOP Publishing: https://doi.org/10.3847/1538-4357/aab718.en_US
dc.identifier.digitalLiu-2018en_US
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aab718en_US
dc.identifier.urihttps://hdl.handle.net/1911/102481en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.subject.keywordhydrodynamicsen_US
dc.subject.keywordplanet–disk interactionsen_US
dc.subject.keywordplanets and satellites: formationen_US
dc.subject.keywordprotoplanetary disksen_US
dc.subject.keywordstars: individual (HD 163296)en_US
dc.subject.keywordturbulenceen_US
dc.titleNew Constraints on Turbulence and Embedded Planet Mass in the HD 163296 Disk from Planet–Disk Hydrodynamic Simulationsen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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