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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/6594
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dc.contributor.authorSubramanian, S-
dc.contributor.authorSubramaniam, A-
dc.date.accessioned2014-04-28T11:54:31Z-
dc.date.available2014-04-28T11:54:31Z-
dc.date.issued2013-
dc.identifier.citationKhare, Pushpa and Ishwara-Chandra C.H., eds., Proceedings of the 31st meeting of the Astronomical Society of India, February 20-22, 2013 , pp. 63 - 66en
dc.identifier.urihttp://hdl.handle.net/2248/6594-
dc.descriptionOpen Accessen
dc.description.abstractThe structural parameters of the Large Magellanic Cloud and the Small Magellanic Cloud are derived from the study of di erent stellar populations, such as, Cepheids (age 100 Myr), Red Clump stars (age 2-9 Gyr) and RR Lyrae stars (age > 9 Gyr). The structural changes of these galaxies as a function of time are identified and the processes which are responsible for these changes are discussed. The formation and early evolution of these two galaxies are found to be di erent.en
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.ispartofseriesAstronomical Society of India Conference Series;9-
dc.relation.urihttp://www.astron-soc.in/bulletin/asics_vol009/en
dc.rights© Astronomical Society of Indiaen
dc.subjectGalaxiesen
dc.subjectMagellanic Cloudsen
dc.subjectStars: Distancesen
dc.subjectStars: Horizontal Branchen
dc.subjectStars: Variablesen
dc.subjectCepheidsen
dc.titleStellar populations in the magellanic cloudsen
dc.typeArticleen
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