Table 6.
Trend of Th/Eu with r-process enrichment.
Star | Eu | Th | (Th/Eu) | Regime 3 | [Eu/Fe] |
---|---|---|---|---|---|
(complete r-process) subclass | |||||
TYC5329-1927-1 | −1 | −1.91 | 0.12 | r-I | 0.89 |
J0858−0809 | −2.41 | −3.07 | 0.22 | r-I | 0.23 |
HD 108317 | −1.37 | −1.99 | 0.24 | r-I | 0.64 |
HD 110184 | −1.91 | −2.5 | 0.26 | r-I | 0.08 |
HE1523−0901 | −0.62 | −1.2 | 0.26 | r-II | 1.86 |
CS22892−052 | −0.86 | −1.42 | 0.28 | r-II | 1.53 |
HD 186478 | −1.34 | −1.85 | 0.31 | r-I | 0.63 |
CS29491−069 | −0.96 | −1.46 | 0.32 | r-II | 1.12 |
RAVEJ203843.2−002333 | −0.75 | −1.24 | 0.32 | r-II | 1.64 |
CS29497−004 | −0.68 | −1.17 | 0.32 | r-II | 1.44 |
J1432−4125 | −1.01 | −1.47 | 0.35 | r-II | 1.44 |
HE0240−0807 | −1.44 | −1.9 | 0.35 | r-I | 0.55 |
BD−155781 | −2.28 | −2.73 | 0.35 | r-I | 0.12 |
HE2224+0143 | −1.02 | −1.47 | 0.35 | r-I | 0.87 |
HE2327−5642( * ) | −1.29 | −1.67 | 0.42 | r-II | 1.07 |
HD 6268( * ) | −1.56 | −1.93 | 0.43 | r-I | 0.54 |
HD 115444( * ) | −1.64 | −1.97 | 0.47 | r-I | 0.68 |
HE2252−4225( * ) | −1.3 | −1.63 | 0.47 | r-II | 1.12 |
CS22953−003( * ) | −1.69 | −1.92 | 0.59 | r-I or r-II | 0.92 |
CS31082−001( * ) | −0.76 | −0.98 | 0.60 | r-II | 1.62 |
CS30315−029( * ) | −2.24 | −2.45 | 0.62 | r-I | 0.67 |
HE1219−0312( * ) | −0.98 | −1.19 | 0.62 | r-II | 1.47 |
redCS31078−018( * ) | −1.17 | −1.35 | 0.66 | r-II | 1.15 |
2MASSJ09544277+5246414( * ) | −1.19 | −1.31 | 0.76 | r-II | 1.28 |
Notes. (Present day) Observed Eu and Th abundances in log ϵ(X) = log(NX/NH + 12) values in low metallicity stars ([Fe/H] < −2.4). The corresponding solar system ratio at the time of its birth (representing the ISM when the solar system got detached) is 0.45 or 0.42 (Lodders et al. 2009; Lodders 2020). Based on their present Th/Eu ratios, the stars with an asterisk would be considered as an actinde-boost stars with Th/Eu > 0.42.
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