论文标题
在λCDM宇宙中模拟Kilonovae
Simulating Kilonovae in the ΛCDM Universe
论文作者
论文摘要
Kilonovae是在中子星星星星合并（NNMS）或中子星光孔合并（NBMS）后产生的光闪光。在这项工作中，我们使用千年模拟，再加上半分析的星系形成模型 - gabe（带有二进制进化的星系组件），该模拟采用了二进制恒星种群合成模型，探索基尔洛诺维奇的宇宙事件率及其宿主星系在宇宙学环境中的特性。我们发现，超新星踢速度为0 km/s的模型最适合观察，但与二进制中子星的某些地层通道一致。这表明NNM更喜欢起源于低踢速度的二进制系统。使用V $ _ {\ rm Kick} $ = 0 km/s，Z = 0时的cosmic事件率为283 GPC $^{ - 3} $ yr $^{ - 1} $和91 Gpc $^{ - 3} $^{ - 3} $ yr $ yr $^$^{ - 1} $，分别是一致的。对于银河系质量星系，我们预测NNM速率为$ 25.7^{+59.6} _ { - 7.1} $ MYR $^{ - 1} $，这也与乳白色中的二元中子星的观察到的属性非常吻合。在银河系质量星系的历史上考虑了所有NNM，我们发现平均的R-Process元素在NNM中的> 79和NBM事件中的收益应为0.01 m $ _ {\ odot} $，以与观察一致。我们得出的结论是，GW170817的宿主星系NGC 4993是NNM的典型宿主星系。但是，通常NNM和NBM倾向于居住在年轻的，蓝色的，形成的，晚期的星系中，分别为$ 10^{10.65} $ M $ _ {\ odot} $和8.72-8.85。通过在宇宙学背景下研究Kilonovae宿主星系，当我们在即将到来的未来有更多事件时，可以更好地限制模型细节。 （简略）
Kilonovae are optical flashes produced in the aftermath of neutron star-neutron star mergers (NNMs) or neutron star-black hole mergers (NBMs). In this work, we use the Millennium Simulation, combined with a semi-analytic galaxy formation model--GABE (Galaxy Assembly with Binary Evolution) which adopts binary stellar population synthesis models, to explore the cosmic event rate of kilonovae, and the properties of their host galaxies in a cosmological context. We find that model with supernova kick velocity of 0 km/s fits the observation best, in agreement with the exception of some formation channels of binary neutron star. This indicates that NNMs prefer to originate from binary systems with low kick velocities. With V$_{\rm kick}$=0 km/s, the cosmic event rate of NNMs and NBMs at z=0 are 283 Gpc$^{-3}$yr$^{-1}$ and 91 Gpc$^{-3}$yr$^{-1}$, respectively, marginally consistent with the constraint from LVC GWTC-1. For Milky Way-mass galaxies, we predict the NNM rate is $25.7^{+59.6}_{-7.1}$ Myr$^{-1}$, which is also in good agreement with the observed properties of binary neutron stars in the Milky Way. Taking all the NNMs into account in the history of Milky Way-mass galaxies, we find that the averaged r-process elements yield with A>79 in a NNM and NBM event should be 0.01 M$_{\odot}$ to be consistent with observation. We conclude that NGC 4993, the host galaxy of GW170817, is a typical host galaxy for NNMs. However, generally NNMs and NBMs tend to reside in young, blue, star-forming, late-type galaxies, with stellar mass and gaseous metallicity distribution peaking at $10^{10.65}$ M$_{\odot}$ and 8.72-8.85, respectively. By studying kilonovae host galaxies in the cosmological background, it is promising to constrain model details better when we have more events in the forthcoming future. (abridged)
