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Stellar Populations in the Magellanic Clouds

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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

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