Table 3.
Abundances of the best-fit models to J0949−1617.
| Model | log ϵ(Eu) | log ϵ(Th) | log ϵ(U) | log(Th/Eu)AGB | log(Th/U)AGB | Δt | δ(Δt′) |
|---|---|---|---|---|---|---|---|
| label | [Gyr] | [Gyr] | |||||
| MAϵ8α08 | −0.98 | −1.27 | −1.68 | −0.29 | 0.40 | 14.95 | −2.25 |
| MAϵ4α08 | −0.99 | −0.92 | −1.16 | 0.07 | 0.24 | 31.80 | −5.89 |
| MAϵ4α04 | −1.08 | −1.12 | −1.63 | −0.05 | 0.51 | 26.16 | 0 |
| MBϵ4α04 | −1.00 | −1.69 | −2.28 | −0.69 | 0.59 | −3.89 | +1.81 |
| MCϵ4α04 | −1.09 | −0.86 | −1.04 | 0.23 | 0.18 | 39.01 | −7.21 |
Notes. We also give the ‘age’ estimate (Δt, i.e., the time since the i-process took place, a lower limit to the stellar age; see text for details) of J0949−1617 based on the Th/Eu abundance ratio and the difference for the age estimate, δ(Δt′), with respect to the MAϵ4α04 model, if relying on the Th/U abundance ratio (see text for details). Note that the age estimate for the MBϵ4α04 model is negative because the Th/Eu ratio in this model is lower than the presently observed ratio. The abundance of U is based solely on the 238U isotope since 235U, with a half-life of t1/2 = 0.7 Gyr, was assumed to have fully decayed.
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