========================================================================== J/A+A/342/881 Uncertainties in r-abundance distribution (Goriely 1999) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1.dat table2.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/342/881 ==========================================================================
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Beginning of ReadMe : J/A+A/342/881 Uncertainties in r-abundance distribution (Goriely 1999) ================================================================================ Uncertainties in the solar system r-abundance distribution Goriely S. <Astron. Astrophys. 342, 881 (1999)> =1999A&A...342..881G ================================================================================ ADC_Keywords: Atomic physics Keywords: nuclear reactions, nucleosynthesis, abundances - Sun: abundances - solar system: general - stars: abundances Description: Tables 1&2 correspond to the first estimate of the error factors affecting the beta decay rates of highly ionized heavy atoms in stellar environments. The uncertainties in the stellar beta-decay and EC rates strongly depend on the relevance of the experimentally unknown transitions at a given temperature and density and the reliability of their evaluated probability. To estimate the temperature- and density-dependent errors on the beta-decay rates, we have reiterated the Yokoi & Takahashi (1987, At. Data Nucl. Data Tables 36, 375) calculation with unknown transition rates modified by a typical error value of log(ft)=+/-0.5 (Takahashi 1998, private communication). No transition faster than log(ft)=5 is permitted in this error calculation. Newly measured transition probabilities, e.g. the allowed transition in the ^187^Re bound-state beta-decay (Bosch et al., 1996PhRvL..77.5190B), have been considered. Minimum and maximum error factors around the published rates of Yokoi & Takahashi (1987) are given in Tables 1 and 2 at temperatures 1<=T_8_<=4 and electronic densities (expressed in terms of 10^26^cm^-3^ of 1<=N_e_<=30. When the density-dependence does not affect the final uncertainty factor by more than 0.10 between the N_e_=1 and 3 cases, only values at N_e_=10 are given in the tables. Note that an increase of transition probability by log(ft)=0.5 gives rise to an increase of the final rate by a maximum value of 3.16. This maximum variation is obtained for many rates. The derived error factors are used in parametric s-process calculations within the canonical multi-event model to estimate their impact on the predicted s-abundance distribution and the resulting uncertainties on the solar r-abundance distribution.