Astronomy and Astrophysics – Astronomy
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...196.4009f&link_type=abstract
American Astronomical Society, 196th AAS Meeting, #40.09; Bulletin of the American Astronomical Society, Vol. 32, p.738
Astronomy and Astrophysics
Astronomy
Scientific paper
Abundances of the most massive stable elements (Os -> Pb or 76 <= Z <= 82) in metal-poor stars can provide crucial information about the so-called ``third neutron-capture peak,'' and are critical to the radioactive-dating technique that uses unstable thorium and uranium as chronometers. As the relevant transitions occur in the UV and are inaccessable to ground-based telescopes, we have obtained high resolution (R ~= 30,000) UV spectra of 10 very metal-poor (--3.0 <= [Fe/H] <= --1.4) halo giants using the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope. Using iterative spectrum synthesis techniques, we derive abundances for some of these heavy elements. We compare our abundances to those predicted for very metal-poor stars based on a scaled solar system rapid-process (production in rapid neutron-capture synthesis events, such as occurs during supernovae explosions). This research is supported by NASA STScI grant GO-08342 and NSF grants AST-9618364 to C.S. and AST-9618332 to J.J.C.
Beers Timothy C.
Cowan John J.
French Rica S.
Lawler James E.
Primas Francesca
No associations
LandOfFree
Neutron-Capture Elements in Very Metal-Poor Halo Stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Neutron-Capture Elements in Very Metal-Poor Halo Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Neutron-Capture Elements in Very Metal-Poor Halo Stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1125385