TY - JOUR
T1 - Circumbinary, not transitional
T2 - On the spiral arms, cavity, shadows, fast radial flows, streamers, and horseshoe in the HD142527 disc
AU - Price, Daniel J.
AU - Cuello, Nicolás
AU - Pinte, Christophe
AU - Mentiplay, Daniel
AU - Casassus, Simon
AU - Christiaens, Valentin
AU - Kennedy, Grant M.
AU - Cuadra, Jorge
AU - Sebastian Perez, M.
AU - Marino, Sebastian
AU - Armitage, Philip J.
AU - Zurlo, Alice
AU - Juhasz, Attila
AU - Ragusa, Enrico
AU - Laibe, Guillaume
AU - Lodato, Giuseppe
N1 - Funding Information:
This project was initiated during the workshop on ‘Planet Formation in the Era of ALMA and Extreme AO’ in Santiago, Chile. Section 2 documents a lengthy discussion between many of us while sharing a sushi lunch. DJP thanks S. Casassus, J. Cuadra, Universidad de Chile, Pontificia Universidad Católica de Chile, and the Millenium Nucleus for their hospitality and financial support during two visits to Santiago. We also thank Yann Boehler, Diego Muñoz, Rebecca Martin, and Rebecca Nealon for useful discussions. DJP is funded by an Australian Research Council Future Fellowship FT13010034 and Discovery Projects DP130102078 and DP180104235. We acknowledge CPU time on Gstar/SwinStar at Swinburne University, funded by the Australian Government, and on the MonARCH cluster at Monash. NC acknowledges financial support from FONDE-CYT grant 3170680. JC and NC acknowledge Millenium Nucleus grant RC130007 (Chilean Ministry of Economy). GMK is supported by the Royal Society as a University Research Fellow. JC acknowledges support from CONICYT-Chile through FONDECYT (1141175) and Basal (PFB0609) grants. We thank the anonymous referee for comments that have improved the paper.
Funding Information:
This projectwas initiated during theworkshop on 'Planet Formation in the Era of ALMA and Extreme AO' in Santiago, Chile. Section 2 documents a lengthy discussion between many of us while sharing a sushi lunch. DJP thanks S. Casassus, J. Cuadra, Universidad de Chile, Pontificia Universidad Cat?lica de Chile, and the Millenium Nucleus for their hospitality and financial support during two visits to Santiago. We also thank Yann Boehler, Diego Mu?oz, Rebecca Martin, and Rebecca Nealon for useful discussions. DJP is funded by an Australian Research Council Future Fellowship FT13010034 and Discovery Projects DP130102078 and DP180104235. We acknowledge CPU time on Gstar/SwinStar at Swinburne University, funded by the Australian Government, and on the MonARCH cluster at Monash. NC acknowledges financial support from FONDECYT grant 3170680. JC and NC acknowledge Millenium Nucleus grant RC130007 (Chilean Ministry of Economy). GMK is supported by the Royal Society as a University Research Fellow. JC acknowledges support from CONICYT-Chile through FONDECYT (1141175) and Basal (PFB0609) grants. We thank the anonymous referee for comments that have improved the paper.
Publisher Copyright:
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2018/6/11
Y1 - 2018/6/11
N2 - We present 3D hydrodynamical models of the HD142527 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 HD142527 disc suggests other mm-bright transition discs showing cavities, spirals, and dust asymmetries may also be explained by the interaction with central companions.
AB - We present 3D hydrodynamical models of the HD142527 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 HD142527 disc suggests other mm-bright transition discs showing cavities, spirals, and dust asymmetries may also be explained by the interaction with central companions.
KW - Accretion
KW - Accretion discs
KW - Binaries: General
KW - Planet-disc interactions
KW - Protoplanetary discs
KW - Submillimetre: Planetary systems
UR - http://www.scopus.com/inward/record.url?scp=85046697082&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty647
DO - 10.1093/mnras/sty647
M3 - Article
AN - SCOPUS:85046697082
SN - 0035-8711
VL - 477
SP - 1270
EP - 1284
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -