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hal.structure.identifierAMOR 2012
dc.contributor.authorTANG, Ya-Wen
hal.structure.identifierAMOR 2012
dc.contributor.authorGUILLOTEAU, S.
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorPIETU, Vincent
hal.structure.identifierAMOR 2012
dc.contributor.authorDUTREY, Anne
dc.contributor.authorOHASHI, Nagayoshi
dc.contributor.authorHO, Paul T. P.
dc.date.created2012-09-25
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnThe circumstellar disk of AB Aurigae has garnered strong attention owing to the apparent existence of spirals at a relatively young stage and also the asymmetric disk traced in thermal dust emission. However, the physical conditions of the spirals are still not well understood. The origin of the asymmetric thermal emission is unclear. We observed the disk at 230 GHz (1.3 mm) in both the continuum and the spectral line ^12CO J=2-1 with IRAM 30-m, the Plateau de Bure interferometer, and the Submillimeter Array to sample all spatial scales from 0.37" to about 50". To combine the data obtained from these telescopes, several methods and calibration issues were checked and discussed. The 1.3 mm continuum (dust) emission is resolved into inner disk and outer ring. Molecular gas at high velocities traced by the CO line is detected next to the stellar location. The inclination angle of the disk is found to decrease toward the center. On a larger scale, based on the intensity weighted dispersion and the integrated intensity map of ^12CO J=2-1, four spirals are identified, where two of them are also detected in the near infrared. The total gas mass of the 4 spirals (M_spiral) is 10^-7 < M_spiral < 10^-5 M_sun, which is 3 orders of magnitude smaller than the mass of the gas ring. Surprisingly, the CO gas inside the spiral is apparently counter-rotating with respect to the CO disk, and it only exhibits small radial motion. The wide gap, the warped disk, and the asymmetric dust ring suggest that there is an undetected companion with a mass of 0.03 M_sun at a radius of 45 AU. Although an hypothetical fly-by cannot be ruled out, the most likely explanation of the AB Aurigae system may be inhomogeneous accretion well above or below the main disk plane from the remnant envelope, which can explain both the rotation and large-scale motions detected with the 30-m image.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enprotoplanetary disks
dc.subject.enstars: formation
dc.subject.enstars: individual: AB
dc.subject.enAurigae
dc.subject.enplanet-disk interactions
dc.title.enThe circumstellar disk of AB Aurigae: evidence for envelope accretion at late stages of star formation?
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201219414
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1209.1299
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A84
bordeaux.volume547
bordeaux.peerReviewedoui
hal.identifierhal-00838682
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00838682v1
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