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оригинального документа
: http://www.mso.anu.edu.au/coala/galaxy.html
Дата изменения: Unknown Дата индексирования: Mon Oct 1 21:18:52 2012 Кодировка: Поисковые слова: п п п п п п п п п п п п п п п р п |
Chiaki Kobayashi, Ralph Sutherland
How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation.
Supernovae feedback drive galactic winds. Supernovae eject not only thermal energy to suppress star formation, but also produce heavy elements to enhance star formation. Therefore, those processes have to be solved simultaneously. In less-massive galaxies, supernova feedback drive galactic winds (Fig. 2.1), and heavy elements are ejected from galaxies into intergalactic medium.
How did our Milky Way Galaxy form? We will perform high-resolution simulations of the Milky Way Galaxy (Fig. 2.2). Comparing the observed kinematics and elemental abundances of stars, we will untangle the formation and evolutionary history of the Milky Way Galaxy (the Galactic Archaeology). This will provide predictions and theoretical interpretations for the next generation of Australian instrument, the multi-object spectrograph HERMES (2012), being developed by the AAO.
Galactic morphology and environmental effect. We will simulate various types of galaxies in different environment: our Milky Way Galaxy, elliptical galaxies, spiral galaxies, and clusters of galaxies. From the comparison with the observed chemical abundances in nearby and distant galaxies, we would like to construct a consistent scenario when and how galaxies form and evolve ("g"alactic archaeology). This will also provide a clue to reveal the origin of the galactic morphology; how did spiral and elliptical galaxies form?
Mapping the kinematics and stellar populations within galaxies. Internal structures are one of the most stringent constraints. With chemodynamical simulations, we can predict those, and will compare with the observations with the ANU's new integral field spectrograph WiFeS and the Giant Magellan Telescope (GMT) (2018?) which Australia is participating.
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