Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4815
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dc.contributor.authorSubramaniam, A-
dc.contributor.authorPrabhu, T. P-
dc.date.accessioned2009-09-11T14:18:03Z-
dc.date.available2009-09-11T14:18:03Z-
dc.date.issued2007-05-24-
dc.identifier.citationDe Jong, R. S. ed., Island Universes: structure and evolution of disk galaxies., Astrophysics and space science proceedings; Vol. 3., pp. 83 - 88en
dc.identifier.isbn978-1-4020-5572-0-
dc.identifier.issn1570-6591-
dc.identifier.urihttp://hdl.handle.net/2248/4815-
dc.descriptionThe original publication is available at springerlink.com-
dc.descriptionRestricted Access-
dc.description.abstractThe stellar radial velocity in the central region of the Large Magellanic Cloud (LMC) is used to estimate the radial velocity curve along various position angles (PA) including the line of nodes (LON). The central part of the radial velocity profile along the LON shows a V-shaped profile instead of a straight line profile. This is a clear indication of counterrotation. To explain the observed velocity profile, we propose the existence of two disks in the inner LMC, with one coun-terrotating. This two disk model is found to match the Hi velocities as well. The presence of a counter-rotating core could be due to internal (secondary bar) / external (gas accretion) origin.en
dc.language.isoenen
dc.publisherSpringeren
dc.relation.ispartofseriesAstrophysics and Space Science Proceedings; Vol. 3-
dc.relation.urihttp://www.springerlink.com/content/u234u75j45005323/en
dc.rights© Springeren
dc.subjectCounterrotating Coreen
dc.subjectLMCen
dc.subjectStellar Radial Velocityen
dc.subjectLarge Magellanic Clouden
dc.subjectLine of Nodesen
dc.titleCounterrotating core in the LMC: accretion and or mergeren
dc.typeArticleen
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