Stellar populations in the magellanic clouds a thesis submitted for the degree of Doctor of Philosophy in Faculty of Science, Calicut University, Calicut, Kerala Smitha Subramanian [Ph.D Thesis]
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TextPublication details: Bangalore Indian Institute of Astrophysics 2011Description: 207pSubject(s): Online resources: Dissertation note: Doctor of Philosophy University of Calicut, Calicut, Kerala 2012 Summary: 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.
| Item type | Current library | Shelving location | Call number | Status | Date due | Barcode |
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Thesis & Dissertations
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IIA Library-Bangalore | General Stacks | (043.2)524.722/ SMI (Browse shelf(Opens below)) | Available | 19243 |
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Thesis Supervisor Dr. Annupurni Subramaniam
Doctor of Philosophy University of Calicut, Calicut, Kerala 2012
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.
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