A 3D hydrodynamics study of gravitational instabilities in a young circumbinary disc. Desai, K., M., Steiman-Cameron, T., Y., Michael, S., Cai, K., & Durisen, R., H. Monthly Notices of the Royal Astronomical Society, 483(2):2347-2361, Oxford University Press, 2019. doi abstract bibtex We present a 3D hydrodynamics study of gravitational instabilities (GIs) in a 0.14 M· circumbinary protoplanetary disc orbiting a 1M· star and a 0.02M· brown dwarf companion. We examine the thermodynamical state of the disc and determine the strengths of GI-induced densitywaves, non-axisymmetric density structures,mass inflowand outflow, and gravitational torques. Results are compared with a parallel simulation of a protoplanetary disc without the brown dwarf binary companion. Simulations are performed using CHYMERA, a radiative 3D hydrodynamics code. The onset of GIs in the circumbinary disc is much more violent due to the stimulation of a strong one-armed density wave by the brown dwarf. Despite this early difference, detailed analyses show that both discs relax to a very similar quasi-steady phase by 2500 years after the beginning of the simulations. Similarities include the thermodynamics of the quasi-steady phase, the final surface density distribution, radial mass influx, and nonaxisymmetric power and torques for spiral arm multiplicities of two or more. Effects of binarity in the disc are evident in gravitational torque profiles, temperature profiles in the inner discs, and radial mass transport. After 3800 years, the semimajor axis of the binary decreases by about one percentage and the eccentricity roughly doubles. The mass transport in the outer circumbinary disc associated with the one-armed wave may influence planet formation.
@article{
title = {A 3D hydrodynamics study of gravitational instabilities in a young circumbinary disc},
type = {article},
year = {2019},
keywords = {Accretion, accretion discs,Binaries: general,Hydrodynamics,Protoplanetary discs},
pages = {2347-2361},
volume = {483},
publisher = {Oxford University Press},
id = {984acb76-a3d4-3b6d-85dd-d31aed777d26},
created = {2020-07-08T14:51:37.938Z},
file_attached = {false},
profile_id = {42d295c0-0737-38d6-8b43-508cab6ea85d},
group_id = {27e0553c-8ec0-31bd-b42c-825b8a5a9ae8},
last_modified = {2020-07-08T14:51:37.938Z},
read = {false},
starred = {false},
authored = {false},
confirmed = {true},
hidden = {false},
private_publication = {false},
abstract = {We present a 3D hydrodynamics study of gravitational instabilities (GIs) in a 0.14 M· circumbinary protoplanetary disc orbiting a 1M· star and a 0.02M· brown dwarf companion. We examine the thermodynamical state of the disc and determine the strengths of GI-induced densitywaves, non-axisymmetric density structures,mass inflowand outflow, and gravitational torques. Results are compared with a parallel simulation of a protoplanetary disc without the brown dwarf binary companion. Simulations are performed using CHYMERA, a radiative 3D hydrodynamics code. The onset of GIs in the circumbinary disc is much more violent due to the stimulation of a strong one-armed density wave by the brown dwarf. Despite this early difference, detailed analyses show that both discs relax to a very similar quasi-steady phase by 2500 years after the beginning of the simulations. Similarities include the thermodynamics of the quasi-steady phase, the final surface density distribution, radial mass influx, and nonaxisymmetric power and torques for spiral arm multiplicities of two or more. Effects of binarity in the disc are evident in gravitational torque profiles, temperature profiles in the inner discs, and radial mass transport. After 3800 years, the semimajor axis of the binary decreases by about one percentage and the eccentricity roughly doubles. The mass transport in the outer circumbinary disc associated with the one-armed wave may influence planet formation.},
bibtype = {article},
author = {Desai, Karna M. and Steiman-Cameron, Thomas Y. and Michael, Scott and Cai, Kai and Durisen, Richard H.},
doi = {10.1093/mnras/sty3240},
journal = {Monthly Notices of the Royal Astronomical Society},
number = {2}
}
Downloads: 0
{"_id":"vWEcvr92QC5eJD85Y","bibbaseid":"desai-steimancameron-michael-cai-durisen-a3dhydrodynamicsstudyofgravitationalinstabilitiesinayoungcircumbinarydisc-2019","authorIDs":[],"author_short":["Desai, K., M.","Steiman-Cameron, T., Y.","Michael, S.","Cai, K.","Durisen, R., H."],"bibdata":{"title":"A 3D hydrodynamics study of gravitational instabilities in a young circumbinary disc","type":"article","year":"2019","keywords":"Accretion, accretion discs,Binaries: general,Hydrodynamics,Protoplanetary discs","pages":"2347-2361","volume":"483","publisher":"Oxford University Press","id":"984acb76-a3d4-3b6d-85dd-d31aed777d26","created":"2020-07-08T14:51:37.938Z","file_attached":false,"profile_id":"42d295c0-0737-38d6-8b43-508cab6ea85d","group_id":"27e0553c-8ec0-31bd-b42c-825b8a5a9ae8","last_modified":"2020-07-08T14:51:37.938Z","read":false,"starred":false,"authored":false,"confirmed":"true","hidden":false,"private_publication":false,"abstract":"We present a 3D hydrodynamics study of gravitational instabilities (GIs) in a 0.14 M· circumbinary protoplanetary disc orbiting a 1M· star and a 0.02M· brown dwarf companion. We examine the thermodynamical state of the disc and determine the strengths of GI-induced densitywaves, non-axisymmetric density structures,mass inflowand outflow, and gravitational torques. Results are compared with a parallel simulation of a protoplanetary disc without the brown dwarf binary companion. Simulations are performed using CHYMERA, a radiative 3D hydrodynamics code. The onset of GIs in the circumbinary disc is much more violent due to the stimulation of a strong one-armed density wave by the brown dwarf. Despite this early difference, detailed analyses show that both discs relax to a very similar quasi-steady phase by 2500 years after the beginning of the simulations. Similarities include the thermodynamics of the quasi-steady phase, the final surface density distribution, radial mass influx, and nonaxisymmetric power and torques for spiral arm multiplicities of two or more. Effects of binarity in the disc are evident in gravitational torque profiles, temperature profiles in the inner discs, and radial mass transport. After 3800 years, the semimajor axis of the binary decreases by about one percentage and the eccentricity roughly doubles. The mass transport in the outer circumbinary disc associated with the one-armed wave may influence planet formation.","bibtype":"article","author":"Desai, Karna M. and Steiman-Cameron, Thomas Y. and Michael, Scott and Cai, Kai and Durisen, Richard H.","doi":"10.1093/mnras/sty3240","journal":"Monthly Notices of the Royal Astronomical Society","number":"2","bibtex":"@article{\n title = {A 3D hydrodynamics study of gravitational instabilities in a young circumbinary disc},\n type = {article},\n year = {2019},\n keywords = {Accretion, accretion discs,Binaries: general,Hydrodynamics,Protoplanetary discs},\n pages = {2347-2361},\n volume = {483},\n publisher = {Oxford University Press},\n id = {984acb76-a3d4-3b6d-85dd-d31aed777d26},\n created = {2020-07-08T14:51:37.938Z},\n file_attached = {false},\n profile_id = {42d295c0-0737-38d6-8b43-508cab6ea85d},\n group_id = {27e0553c-8ec0-31bd-b42c-825b8a5a9ae8},\n last_modified = {2020-07-08T14:51:37.938Z},\n read = {false},\n starred = {false},\n authored = {false},\n confirmed = {true},\n hidden = {false},\n private_publication = {false},\n abstract = {We present a 3D hydrodynamics study of gravitational instabilities (GIs) in a 0.14 M· circumbinary protoplanetary disc orbiting a 1M· star and a 0.02M· brown dwarf companion. We examine the thermodynamical state of the disc and determine the strengths of GI-induced densitywaves, non-axisymmetric density structures,mass inflowand outflow, and gravitational torques. Results are compared with a parallel simulation of a protoplanetary disc without the brown dwarf binary companion. Simulations are performed using CHYMERA, a radiative 3D hydrodynamics code. The onset of GIs in the circumbinary disc is much more violent due to the stimulation of a strong one-armed density wave by the brown dwarf. Despite this early difference, detailed analyses show that both discs relax to a very similar quasi-steady phase by 2500 years after the beginning of the simulations. Similarities include the thermodynamics of the quasi-steady phase, the final surface density distribution, radial mass influx, and nonaxisymmetric power and torques for spiral arm multiplicities of two or more. Effects of binarity in the disc are evident in gravitational torque profiles, temperature profiles in the inner discs, and radial mass transport. After 3800 years, the semimajor axis of the binary decreases by about one percentage and the eccentricity roughly doubles. The mass transport in the outer circumbinary disc associated with the one-armed wave may influence planet formation.},\n bibtype = {article},\n author = {Desai, Karna M. and Steiman-Cameron, Thomas Y. and Michael, Scott and Cai, Kai and Durisen, Richard H.},\n doi = {10.1093/mnras/sty3240},\n journal = {Monthly Notices of the Royal Astronomical Society},\n number = {2}\n}","author_short":["Desai, K., M.","Steiman-Cameron, T., Y.","Michael, S.","Cai, K.","Durisen, R., H."],"biburl":"https://bibbase.org/service/mendeley/42d295c0-0737-38d6-8b43-508cab6ea85d","bibbaseid":"desai-steimancameron-michael-cai-durisen-a3dhydrodynamicsstudyofgravitationalinstabilitiesinayoungcircumbinarydisc-2019","role":"author","urls":{},"keyword":["Accretion","accretion discs","Binaries: general","Hydrodynamics","Protoplanetary discs"],"metadata":{"authorlinks":{}},"downloads":0},"bibtype":"article","creationDate":"2020-07-09T06:42:37.003Z","downloads":0,"keywords":["accretion","accretion discs","binaries: general","hydrodynamics","protoplanetary discs"],"search_terms":["hydrodynamics","study","gravitational","instabilities","young","circumbinary","disc","desai","steiman-cameron","michael","cai","durisen"],"title":"A 3D hydrodynamics study of gravitational instabilities in a young circumbinary disc","year":2019,"biburl":"https://bibbase.org/service/mendeley/42d295c0-0737-38d6-8b43-508cab6ea85d","dataSources":["zgahneP4uAjKbudrQ","ya2CyA73rpZseyrZ8","2252seNhipfTmjEBQ"]}