English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/18585
Share/Impact:
Statistics
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:

DC FieldValueLanguage
dc.contributor.authorMontuori, M.-
dc.contributor.authorCapuzzo-Dolcetta, R.-
dc.contributor.authorMatteo, P. di-
dc.contributor.authorLepinette, Alain-
dc.contributor.authorMiocchi, P.-
dc.date.accessioned2009-11-12T12:25:43Z-
dc.date.available2009-11-12T12:25:43Z-
dc.date.issued2007-04-20-
dc.identifier.citationAstrophysical Journal 659(2): 1212-1221 (2007)en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10261/18585-
dc.description10 pages, 8 figures, 3 tables, 1 appendix.-- See also http://www.sdss.org.en_US
dc.description.abstractWe present the results of detailed N-body simulations of clusters moving in a realistic Milky Way (MW) potential. The strong interaction with the bulge and the disk of the Galaxy leads to the formation of tidal tails, emanating from opposite sides of the cluster. Some characteristic features in the morphology and orientation of these streams are recognized and interpreted. The tails have a complex morphology, particularly when the cluster approaches its apogalacticon, showing multiple "arms" in remarkable similarity to the structures observed around NGC 288 and Willman 1. Actually, the tails are generally good tracers of the cluster path quite far from the cluster center (>7-8 tidal radii), while on the smaller scale they are mainly pointing in the direction of the Galaxy center. In particular, the orientation of the inner part of the tails is highly correlated with the cluster orbital phase and the local orbital angular acceleration. This implies that, in general, the orbital path cannot be estimated directly from the orientation of the tails, unless a sufficient large field around the cluster is availableen_US
dc.format.extent594880 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.publisherAmerican Astronomical Societyen_US
dc.rightsopenAccessen_US
dc.subjectGalaxiesen_US
dc.subjectGlobular clustersen_US
dc.subjectN-body simulationsen_US
dc.titleTidal tails around globular clusters: Are they a good tracer of cluster orbits?en_US
dc.typeartículoen_US
dc.identifier.doihttp://dx.doi.org/10.1086/512114-
dc.description.peerreviewedPeer revieweden_US
dc.relation.publisherversionhttp://dx.doi.org/10.1086/512114en_US
Appears in Collections:(CAB) Artículos
Files in This Item:
File Description SizeFormat 
70729.web.pdf580,94 kBAdobe PDFThumbnail
View/Open
Show simple item record
 

Related articles:


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.