1 / 8

Anna Frebel University of Texas at Austin anna@astro.as.utexas

Explore the oldest stars in the Milky Way through abundance analysis, focusing on r-process enhanced stars. Learn how the chemical "fingerprint" of nucleosynthesis events unveils the Universe's past. Discover the methods behind identifying and studying metal-poor stars through spectroscopy. Delve into the mystery of Pop III stars and their significance in our understanding of galactic evolution and stellar populations.

kevinmorris
Download Presentation

Anna Frebel University of Texas at Austin anna@astro.as.utexas

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Abundance analysis of bright metal-poor stars from the Hamburg/ESO surveyorThe oldest stars in the Galaxy Anna Frebel University of Texas at Austin anna@astro.as.utexas.edu

  2. Spectral Comparison [Fe/H]=0 [Fe/H]=-4 [Fe/H]=-5.3 Pop III star (just noise…?!?) Christlieb 2003

  3. Three Observational Steps to Find Metal-Poor Stars • Sample selection and visual • inspection: • Find appropriate candidates • 2. Follow-up spectroscopy • (medium resolution): • Derive estimate for [Fe/H] • from the Ca II K line • 3. High-resolution • spectroscopy: • Detailed abundances analysis Frebel et al. 2005b

  4. Abundances of HE 1523−0901 Frebel et al. (2007), in prep.

  5. r-Process Enhanced Stars(rapid neutron-capture process) • Responsible for the production of heavy elements • ~5% among metal-poor stars with [Fe/H] <  2.5 => Only ~12 stars known so far with [r/Fe] > 1.0 • Chemical “fingerprint” of previous nucleosynthesis event • Possible production sites: SN type II, neutrino-driven winds • Nucleo-chronometry: with Th, U and stable r-process elements (Eu, Os, Ir)

  6. U II at 3859Å Frebel et al. (2007), ApJL submitted

  7. The r-Process Pattern scaled solar r-process pattern HE 1523-0901

  8. The Age of HE 1523−0901 Age:

More Related