BEGIN:VCALENDAR VERSION:2.0 PRODID:-//ZContent.net//ZapCalLib 1.0//EN CALSCALE:GREGORIAN METHOD:PUBLISH BEGIN:VEVENT DTSTART;TZID=Atlantic/Canary:20131003T103000 DTEND;TZID=Atlantic/Canary:20131003T113000 UID:iactalks-543 X-WR-CALNAME: IAC Talks: Open Astronomy Seminars X-ORIGINAL-URL: /iactalks/Talks/view/543 CREATED:2013-10-03T10:30:00+01:00 X-WR-CALDESC: IAC Talks upcomming talks SUMMARY:Star formation modes and population gradients in simulated dwarf ga laxies DESCRIPTION:Star formation modes and population gradients in simulated dwar f galaxies \nDr. Joery Schroyen\n\nToday we largely understand the large s cale evolution of the Universe but we have only little knowledge of the sm all scale physics involved in forming and evolving the baryonic structure (gas, stars and dust) of galaxies. Dwarf galaxies are considerd to be the ideal ”galactic laboratories” to gain insight into the astroph ysical processes governing galaxy evolution in general. The obvious main f eature of a dwarf galaxy is, that it is small - about 1/10 of the Milky Wa y’s size. Their relatively shallow gravitational potential makes the m very sensitive to the different (astro)physical processes that affect ga laxy evolution and counteract gravity. Hence we can use these galaxies to try to understand and answer the questions we still have about how, when a nd why galaxies form stars, stop forming stars, and recycle stellar-synthe sised elements in the interstellar medium. Experimenting in these “g alactic laboratories” is of course confined to the virtual universe, which we do by running state- of-the-art Nbody-SPH simulations of dwarf g alaxy formation and evolution. Due to their small dimensions, these can ac hieve much higher resolution and physical detail than any other type of ga lactic simulations. In this talk, I will discuss the main prop- erties/par ameters determining the behaviour and appearance of the dwarf galaxy model s, and use the results to compare with and explain observations. END:VEVENT END:VCALENDAR