Shell galaxies are usually ellipticals with concentric faint arc-like stellar structures with sharp outer edges. They originate from galactic collisions (so called mergers). According to observations, some galaxies has also gaseous structures, that can be associated with stellar shells. We carry out a few numerical simulations, in which we recreate gaseous shells throug radial collisions of small and large elliptical galaxies. Then we analyze the differences between stellar and gaseous shells. Our simulations are based on earlier models, which describes gas by using so called "sticky-particles" hydrodynamics. This approach was so far quite succesful in resolving origin of gaseous shells. Our conclusion is, that gas in preset galaxies is not sufficient to make any difference. Higher quantities on the other hand has significant effect. Powered by TCPDF (www.tcpdf.org)
| Identifer | oai:union.ndltd.org:nusl.cz/oai:invenio.nusl.cz:347204 |
| Date | January 2015 |
| Creators | Zimandl, Martin |
| Contributors | Jungwiert, Bruno, Šolc, Martin |
| Source Sets | Czech ETDs |
| Language | Czech |
| Detected Language | English |
| Type | info:eu-repo/semantics/masterThesis |
| Rights | info:eu-repo/semantics/restrictedAccess |
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