r-process abundances in neutron star merger dynamical ejecta given different fission yields

This data release contains nucleosynthesis predictions following Vassh et al. (2020) for the r-process abundances of binary neutron star merger ejecta based on the simulation trajectories of Radice et al. (2018), which were mapped to parametrized trajectories based on their neutron-richness (Ye), entropy (s), and expansion timescale (tau). The neutron star merger scenarios considered here cover a wide range of neutron star masses. Calculations were performed with the PRISM code (Mumpower et al. 2018) which accounts for nuclear reheating. Results are reported for two fission yield sets, the Finite Range Liquid Drop Model (FRLDM, Mumpower et al. 2020) and 50/50 symmetric splits. All calculations assumed FRDM12 (Möller et al. 2016) for the nuclear mass model and apply the SFHO equation of state when obtaining the initial composition from nuclear statistical equilibrium (NSE). When using these nucleosynthesis yields, please cite this Zenodo data release (Vassh 2022). Refer to Vassh et al. (2020) for further details on the nuclear physics inputs, to Mumpower et al. (2018) for further details on FRLDM, and to Radice et al. (2018) for further details on the merger ejecta trajectories.

本数据集发布包含基于Radice等人（2018）的模拟轨迹所得到的双中子星并合抛射物快中子俘获过程（r-process）丰度核合成预言，该预言遵循Vassh等人（2020）的研究方法。上述模拟轨迹被转换为基于富中子度（Ye）、熵（s）以及膨胀时标（τ）的参数化轨迹。

本次研究涵盖的中子星并合场景覆盖了大范围的中子星质量区间。所有计算均采用考虑核再加热过程的PRISM代码（Mumpower等人2018）完成。

研究结果基于两组裂变产额集合进行呈现：一是有限程液滴模型（FRLDM，Mumpower等人2020），二是50/50对称分裂方案。

所有计算均采用FRDM12（Möller等人2016）作为核质量模型，且在通过核统计平衡（NSE）获取初始成分时，使用SFHO状态方程。

若使用本次发布的核合成产额数据，请引用本Zenodo数据集发布（Vassh 2022）。如需了解核物理输入参数的更多细节，请参阅Vassh等人（2020）；如需了解FRLDM的更多细节，请参阅Mumpower等人（2018）；如需了解并合抛射物轨迹的更多细节，请参阅Radice等人（2018）。