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Planet Formation in AB Aurigae: Imaging of the inner gaseous Spirals observed inside the Dust Cavity

hal.structure.identifierState Key Laboratory of Metal Matrix Composites
dc.contributor.authorTANG, Ya-Wen
hal.structure.identifierAMOR 2017
dc.contributor.authorGUILLOTEAU, S.
hal.structure.identifierAMOR 2017
dc.contributor.authorDUTREY, Anne
dc.contributor.authorMUTO, Takayuki
hal.structure.identifierBeijing National Laboratory for Condensed Matter Physics
dc.contributor.authorSHEN, Bo-Ting
hal.structure.identifierDepartment of Genetics
dc.contributor.authorGU, Pin-Gao
hal.structure.identifierNagoya University
dc.contributor.authorINUTSUKA, Shu-Ichiro
hal.structure.identifierIbaraki University
dc.contributor.authorMOMOSE, Munetake
dc.contributor.authorPIETU, Vincent
dc.contributor.authorFUKAGAWA, Misato
hal.structure.identifierAMOR 2017
dc.contributor.authorCHAPILLON, E.
dc.contributor.authorHO, Paul T. P.
hal.structure.identifierAMOR 2017
dc.contributor.authorDI FOLCO, E.
dc.contributor.authorCORDER, Stuartt
hal.structure.identifierNational Institute for Materials Science [NIMS]
dc.contributor.authorOHASHI, Nagayoshi
dc.contributor.authorHASHIMOTO, Jun
dc.date.issued2017-04
dc.identifier.issn0004-637X
dc.description.abstractEnWe report the results of ALMA observations of a protoplanetary disk surrounding the Herbig Ae star AB Aurigae. We obtained high-resolution (0.1"; 14 au) images in $^{12}$CO (J=2-1) emission and in dust continuum at the wavelength of 1.3 mm. The continuum emission is detected at the center and at the ring with a radius of $\sim$ 120 au. The CO emission is dominated by two prominent spirals within the dust ring. These spirals are trailing and appear to be about 4 times brighter than their surrounding medium. Their kinematics is consistent with Keplerian rotation at an inclination of 23 degree. The apparent two-arm-spiral pattern is best explained by tidal disturbances created by an unseen companion located at 60--80 au, with dust confined in the pressure bumps created outside this companion orbit. An additional companion at r of 30 au, coinciding with the peak CO brightness and a large pitch angle of the spiral, would help to explain the overall emptiness of the cavity. Alternative mechanisms to excite the spirals are discussed. The origin of the large pitch angle detected here remain puzzling.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enPlanet Formation in AB Aurigae: Imaging of the inner gaseous Spirals observed inside the Dust Cavity
dc.typeArticle de revue
dc.identifier.doi10.3847/1538-4357/aa6af7
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1704.02699
bordeaux.journalThe Astrophysical Journal
bordeaux.pageid. 32
bordeaux.volume840
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-01509538
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01509538v1
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