Reference : Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flow...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/225414
Circumbinary, not transitional: on the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD 142527 disc
English
Price, Daniel J. [Monash Centre for Astrophysics (MoCA) and School of Physics and Astronomy, Monash University, Clayton, Vic 3800, Australia <ID system="ORCID">0000-0002-4716-4235</ID>]
Cuello, Nicolás [Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; Instituto de Astrofísica, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile; Núcleo Milenio de Formación Planetaria (NPF), Chile <ID system="ORCID">0000-0003-3713-8073</ID>]
Pinte, Christophe [Monash Centre for Astrophysics (MoCA) and School of Physics and Astronomy, Monash University, Clayton, Vic 3800, Australia; Univ. Grenoble Alpes, CNRS, IPAG/UMR 5274, F-38000 Grenoble, France]
Mentiplay, Daniel [Monash Centre for Astrophysics (MoCA) and School of Physics and Astronomy, Monash University, Clayton, Vic 3800, Australia]
Casassus, Simon [Instituto de Astrofísica, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile; Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile]
Christiaens, Valentin mailto [Université de Liège - ULiège > > > Form. doct. sc. (sc. spatiales - paysage)]
Kennedy, Grant M. [Institute of Astronomy, University of Cambridge, Madingley Rd, Cambridge CB3 0HA, UK <ID system="ORCID">0000-0001-6831-7547</ID>]
Cuadra, Jorge [Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; Instituto de Astrofísica, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile; Núcleo Milenio de Formación Planetaria (NPF), Chile]
Sebastian Perez, M. [Instituto de Astrofísica, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile; Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile]
Marino, Sebastian [Institute of Astronomy, University of Cambridge, Madingley Rd, Cambridge CB3 0HA, UK <ID system="ORCID">0000-0002-5352-2924</ID>]
Armitage, Philip J. [JILA, University of Colorado and NIST, 440 UCB, Boulder, CO 80309-0440, USA; Department of Astrophysical and Planetary Sciences, University of Colorado, 391 UCB, Boulder, CO 80309-0391, USA]
Zurlo, Alice [Instituto de Astrofísica, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile; Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile]
Juhasz, Attila [Institute of Astronomy, University of Cambridge, Madingley Rd, Cambridge CB3 0HA, UK]
Ragusa, Enrico [Dipartimento di Fisica, Università Degli Studi di Milano, Via Celoria 16, I-20133 Milano, Italy <ID system="ORCID">0000-0001-5378-7749</ID>]
Laibe, Guillaume [Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis-Laval, France]
Lodato, Giuseppe [Dipartimento di Fisica, Università Degli Studi di Milano, Via Celoria 16, I-20133 Milano, Italy)]
1-Jun-2018
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
477
1270-1284
Yes (verified by ORBi)
International
0035-8711
1365-2966
Oxford
United Kingdom
[en] accretion ; accretion discs ; planet-disc interactions ; protoplanetary discs ; binaries: general ; submillimetre: planetary systems
[en] We present 3D hydrodynamical models of the HD 142527 protoplanetary disc, a bright and well-studied disc that shows spirals and shadows in scattered light around a 100 au gas cavity, a large horseshoe dust structure in mm continuum emission, together with mysterious fast radial flows and streamers seen in gas kinematics. By considering several possible orbits consistent with the observed arc, we show that all of the main observational features can be explained by one mechanism - the interaction between the disc and the observed binary companion. We find that the spirals, shadows, and horseshoe are only produced in the correct position angles by a companion on an inclined and eccentric orbit approaching periastron - the `red' family from Lacour et al. Dust-gas simulations show radial and azimuthal concentration of dust around the cavity, consistent with the observed horseshoe. The success of this model in the HD 142527 disc suggests other mm-bright transition discs showing cavities, spirals, and dust asymmetries may also be explained by the interaction with central companions.
http://hdl.handle.net/2268/225414
10.1093/mnras/sty647
http://cdsads.u-strasbg.fr/abs/2018MNRAS.477.1270P

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