Detectability of compact binary merger macronovae
Detectability of compact binary merger macronovae
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DOI：
10.1088/1361-6382/aa68a9
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发表时间：
2016-11
影响因子：
3.5
通讯作者：
S. Rosswog;U. Feindt;O. Korobkin;Meng-Ru Wu;J. Sollerman;A. Goobar;G. Martínez-Pinedo
中科院分区：
文献类型：
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作者：
S. Rosswog;U. Feindt;O. Korobkin;Meng-Ru Wu;J. Sollerman;A. Goobar;G. Martínez-Pinedo
我们研究双中子星和中子星黑洞合并后发生的放射性电磁瞬变（“巨新星”）的光学和近红外光度以及可检测性。我们探索动态喷射物和不同类型的风流出引起的瞬变。基于完整的核网络模拟，我们计算了不同波段的光变曲线。我们通过比较（a）两个不同的核反应网络和（b）两个宏新星模型来审查结果的稳健性。我们特别探讨了结果对 α 衰变反式铅核的产生有多敏感。我们比较了两种常用的质量模型：有限范围液滴模型 (FRDM) 和 Duflo 和 Zuker 的核质量模型 (DZ31)。我们发现α衰变反式铅核的丰度对由此产生的巨新星的可观测性有重大影响。例如，DZ31 模型产生相当大的丰度，从而导致更大的加热速率和热化效率，因此预测更亮的宏新星瞬变。我们发现，NSNS 模型的动态喷射物可以达到超过 -15 的峰值 K 波段震级，而 NSBH 模型的动态喷射物可以达到 -16 以上。我们的一些风力模型可以达到类似的值。我们的几个模型（风模型和动力喷射物）产生的特性与短 GRB 130603B 后观察到的瞬态类似。我们进一步探索当前和未来仪器（例如 VISTA、ZTF 和 LSST）的预期宏新星探测频率。
We study the optical and near-infrared luminosities and detectability of radioactively powered electromagnetic transients (‘macronovae’) occuring in the aftermath of binary neutron star and neutron star black hole mergers. We explore the transients that result from the dynamic ejecta and those from different types of wind outflows. Based on full nuclear network simulations we calculate the resulting light curves in different wavelength bands. We scrutinize the robustness of the results by comparing (a) two different nuclear reaction networks and (b) two macronova models. We explore in particular how sensitive the results are to the production of α-decaying trans-lead nuclei. We compare two frequently used mass models: the finite-range Droplet model (FRDM) and the nuclear mass model of Duflo and Zuker (DZ31). We find that the abundance of α-decaying trans-lead nuclei has a significant impact on the observability of the resulting macronovae. For example, the DZ31 model yields considerably larger abundances resulting in larger heating rates and thermalization efficiencies and therefore predicts substantially brighter macronova transients. We find that the dynamic ejecta from NSNS models can reach peak K-band magnitudes in excess of −15 while those from NSBH cases can reach beyond −16. Similar values can be reached by some of our wind models. Several of our models (both wind and dynamic ejecta) yield properties that are similar to the transient that was observed in the aftermath of the short GRB 130603B. We further explore the expected macronova detection frequencies for current and future instruments such as VISTA, ZTF and LSST.