Colloquia and PhD Talks Schedule Summer 2014
Qualifying Exam/2nd Year Defense "Outflows and Chemical Enrichment from Clustered Supernovae in the First Galaxies" University of Texas at Austin Qualifying Exam Committee Meeting follows at 4 PM in RLM 15.216A |
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Qualifying Exam/2nd Year Defense "The Lyman-alpha Signature of the First Galaxies" University of Texas at Austin Qualifying Exam Committee Meeting follows at 3 PM in RLM 15.216A |
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Qualifying Exam/2nd Year Defense "Formation of Massive Star Clusters - an Application of Monte Carlo Radiation Hydrodynamics" University of Texas at Austin Qualifying Exam Committee Meeting follows at 3 PM in RLM 15.202A |
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Special Seminar "Fragmentation in Primordial Gas: Improving H2 Cooling and Self-Shielding" University of Heidelberg, Germany (host: Volker Bromm) |
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Special Visiting Speaker Presentation (visiting: 7-14 June 2014) "Pre-supernova Convection in Massive Stars" University of Chicago host: Crag Wheeler |
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PhD Defense Presentation "Creating and Measuring White Dwarf Photospheres in a Terrestrial Laboratory" University of Texas at Austin PhD Committee Meeting follows at 12 Noon in RLM 15.216A |
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PhD Defense Presentation "Study of Galactic Clumps with Millimeter/Submillimeter Continuum and Molecular Emission: Early Stages of Massive Star Formation" University of Texas at Austin PhD Committee Meeting follows at 4 PM in RLM 15.216A |
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PhD Defense Presentation "Simulating the Formation, Properties, and Impact of Stellar Systems in the First Galaxies" University of Texas at Austin PhD Committee Meeting follows at 12 Noon in RLM 15.216A |
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Special Presentation "The Violent Early Lives of Stars and Planets" We typically envision the formation process of young stars to be a sequence from collapsing core, to protostar surrounded by an envelope, to a young star with a surrounding disk, and finally planets. The dearth of luminous young stars and the rare but dramatic bursts (FU Orionis outbursts) seen in others is shifting the paradigm to an episodic picture of accretion. If common to most young star systems, the aftereffects of FU Orionis outbursts set the initial conditions for the epoch of planet formation, creating irreversible effects on composition and altering the disk mass available to make planets. The unprecedented capabilities of JWST-MIRI, as well as widespread IR monitoring, is required to identify bursts in progress and to understand the triggering cause. Are the final properties of protoplanetary disks set primarily by the composition of their local cloud, or by the timing of the final outburst? University of Texas at Austin |
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PhD Defense Presentation "The Chemical Abundances of Stars in the Halo" University of Texas at Austin PhD Committee Meeting follows at 12 Noon in RLM 15.202A |
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PhD Defense Presentation "Radiation Hydrodynamics and Simulations of Astrophysical Phenomena" University of Texas at Austin PhD Committee Meeting follows at 4 PM in RLM 15.202A |
Visitors to the Department of Astronomy can find detailed information and maps on our Visiting Austin Page.
Please report omissions/corrections to: G. Orris at argus@astro.as.utexas.edu.
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