Stellar Populations in the Magellanic Clouds

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/6545

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DC Field	Value	Language
dc.contributor.author	Smitha, S	-
dc.date.accessioned	2014-02-07T10:02:07Z	-
dc.date.available	2014-02-07T10:02:07Z	-
dc.date.issued	2011-08	-
dc.identifier.citation	Ph.D. Thesis, Calicut University, Calicut	en
dc.identifier.uri	http://hdl.handle.net/2248/6545	-
dc.description	Thesis Supervisor Dr.Annapurni Subramaniam	en
dc.description.abstract	The Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) are two nearby galaxies located at a distance of 50 kpc and 60 kpc respectively. The Magellanic Clouds (MCs) host young, intermediate-age and old stellar populations. In this study, the stellar populations in the MCs are used as a tool to understand the structure and evolution of these galaxies as well as to understand the evolution of the Magellanic system as a whole. The structure of the MCs are studied using stellar populations (standard candles) of different ages (Cepheids - 100 Myr, Red clump stars: 2-9 Gyr & RR Lyrae stars > 9 Gyr) and the quantitative estimates of the structural parameters are derived. This study reveals the structural changes in the two galaxies as a function of time, and help to identify processes like interactions as well as mergers experienced by MCs at different epochs.	en
dc.language.iso	en	en
dc.publisher	Indian Institute of Astrophysics	en
dc.rights	© Indian Institute of Astrophysics	en
dc.title	Stellar Populations in the Magellanic Clouds	en
dc.type	Thesis	en
Appears in Collections:	IIAP Ph.D.Theses

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