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Article: Possible molecular spiral arms in the protoplanetary disk of AB aurigae

TitlePossible molecular spiral arms in the protoplanetary disk of AB aurigae
Authors
KeywordsPlanetary Systems: Protoplanetary Disks
Stars: Individual (Ab Aur)
Issue Date2006
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2006, v. 645 n. 2 I, p. 1297-1304 How to Cite?
AbstractThe circumstellar dust disk of the Herbig Ae star AB Aur has been found to exhibit complex spiral-like structures in the near-IR image obtained with the Subaru Telescope. We present maps of the disk in both 12CO (3-2) and dust continuum at 345 GHz with the Submillimeter Array at an angular resolution of 1″.0 × 0″.7 (144 × 100 AU). The continuum emission traces a dust disk with a central depression and a maximum overall dimension of 450 AU (FWHM). This dust disk exhibits several distinct peaks that appear to coincide with bright features in the near-IR image, in particular the brightest inner spiral arm. The CO emission traces a rotating gas disk of size 530 × 330 AU with a deprojected maximum velocity of 2.8 km s -1 at 450 AU. In contrast with the dust disk, the gas disk exhibits an intensity peak at the stellar position. Furthermore, the CO emission in several velocity channels traces the innermost spiral arm seen in the near-IR. We compare the observed spatial-kinematic structure of the CO emission to a simple model of a disk in Keplerian rotation and find that only the emission tracing the main spiral arm clearly lies outside the confines of our model. This emission has a net outward radial motion compared with the radial velocity predicted by the model at the location of the main spiral arms. The disk of AB Aur is therefore quite different from the Keplerian disks seen around many Herbig Ae stars. The spiral-like structures of the disk with non-Keplerian motions we revealed in 12CO (3-2), together with the central depression of the dust disk, could be explained to be driven by the possible existence of a giant planet forming in the disk. © 2006. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175024
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLin, SYIen_US
dc.contributor.authorOhashi, Nen_US
dc.contributor.authorLim, Jen_US
dc.contributor.authorHo, PTPen_US
dc.contributor.authorFukaoawa, Men_US
dc.contributor.authorTamura, Men_US
dc.date.accessioned2012-11-26T08:48:49Z-
dc.date.available2012-11-26T08:48:49Z-
dc.date.issued2006en_US
dc.identifier.citationAstrophysical Journal Letters, 2006, v. 645 n. 2 I, p. 1297-1304en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175024-
dc.description.abstractThe circumstellar dust disk of the Herbig Ae star AB Aur has been found to exhibit complex spiral-like structures in the near-IR image obtained with the Subaru Telescope. We present maps of the disk in both 12CO (3-2) and dust continuum at 345 GHz with the Submillimeter Array at an angular resolution of 1″.0 × 0″.7 (144 × 100 AU). The continuum emission traces a dust disk with a central depression and a maximum overall dimension of 450 AU (FWHM). This dust disk exhibits several distinct peaks that appear to coincide with bright features in the near-IR image, in particular the brightest inner spiral arm. The CO emission traces a rotating gas disk of size 530 × 330 AU with a deprojected maximum velocity of 2.8 km s -1 at 450 AU. In contrast with the dust disk, the gas disk exhibits an intensity peak at the stellar position. Furthermore, the CO emission in several velocity channels traces the innermost spiral arm seen in the near-IR. We compare the observed spatial-kinematic structure of the CO emission to a simple model of a disk in Keplerian rotation and find that only the emission tracing the main spiral arm clearly lies outside the confines of our model. This emission has a net outward radial motion compared with the radial velocity predicted by the model at the location of the main spiral arms. The disk of AB Aur is therefore quite different from the Keplerian disks seen around many Herbig Ae stars. The spiral-like structures of the disk with non-Keplerian motions we revealed in 12CO (3-2), together with the central depression of the dust disk, could be explained to be driven by the possible existence of a giant planet forming in the disk. © 2006. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectPlanetary Systems: Protoplanetary Disksen_US
dc.subjectStars: Individual (Ab Aur)en_US
dc.titlePossible molecular spiral arms in the protoplanetary disk of AB aurigaeen_US
dc.typeArticleen_US
dc.identifier.emailLim, J: jjlim@hku.hken_US
dc.identifier.authorityLim, J=rp00745en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/504368en_US
dc.identifier.scopuseid_2-s2.0-33746890868en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-33746890868&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume645en_US
dc.identifier.issue2 Ien_US
dc.identifier.spage1297en_US
dc.identifier.epage1304en_US
dc.identifier.isiWOS:000239053900045-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLin, SYI=8267453900en_US
dc.identifier.scopusauthoridOhashi, N=44561415400en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridHo, PTP=7402211489en_US
dc.identifier.scopusauthoridFukaoawa, M=14059877900en_US
dc.identifier.scopusauthoridTamura, M=7403258846en_US

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