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 |