R-process pattern in the Very-Metal-Poor Halo Star CS31082-001

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dc.creatorHill, V.
dc.creatorPlez, B.
dc.creatorCayrel, R.
dc.creatorBeers, T. C.
dc.date2001-04-10
dc.date.accessioned2026-07-07T01:58:11Z
dc.date.available2026-07-07T01:58:11Z
dc.descriptionThe very-metal-poor halo star CS31082-001 was discovered to be very strongly r-process-enhanced during the course of a VLT+UVES high-resolution follow-up of metal-poor stars identified in the HK survey of Beers and colleagues. Both the strong n-capture element enhancement and the low carbon and nitrogen content of the star (reducing the CN molecular band contamination) led to the first $^{238}$U abundance measurement in a stellar spectrum (Cayrel et al. 2001), and the opportunity to use both radioactive species $^{238}$U and $^{232}$Th for dating the progenitor to this star. However, age computations all rely on the hypothesis that the r-process pattern is solar, as this was indeed observed in the other famous r-process-enhanced very metal poor stars CS22892-052 (Sneden et al. 1996, 2000) and in HD115444 (Westin et al. 2000). Here, we investigate whether this hypothesis is verified also for CS31082-001, using a preliminary analysis of over 20 abundances of n-capture elements in the range Z=38 to Z=92.
dc.description3 pages, 2 figures. To appear in `Astrophysical Ages and Timescales' ASP Conf. Ser., Eds. T. von Hippel, N. Manset, C. Simpson
dc.identifierhttps://arxiv.org/abs/astro-ph/0104172
dc.identifierhttp://arxiv.org/abs/astro-ph/0104172
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2672
dc.subjectAstrophysics
dc.titleR-process pattern in the Very-Metal-Poor Halo Star CS31082-001
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