Symmetry energy constraints from GW170817 and laboratory experiments
Symmetry energy constraints from GW170817 and laboratory experiments
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DOI：
10.1016/j.physletb.2019.06.059
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发表时间：
2019-06
影响因子：
4.4
通讯作者：
M. Tsang;W. G. Lynch;P. Danielewicz;C. Tsang
中科院分区：
文献类型：
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作者：
M. Tsang;W. G. Lynch;P. Danielewicz;C. Tsang
LIGO-Virgo 合作探测双中子星合并事件 GW170817，扩大了对核物质状态方程 (EoS) 的理解。这些测量结果为总压力提供了新的限制，但没有阐明其起源，因为没有区分对称能量对压力的贡献，对称能量控制着中子星的大部分内部结构。通过结合从GW170817事件中提取的中子星EoS和核-核碰撞实验中对称物质的EoS，我们提取了对称压力，即中子和核物质在1.2 ρ 0 到4.5 ρ 0 密度区域上的压力差。虽然对称压力的不确定性很大，但可以通过新的实验和天体物理结果来降低。
The LIGO-Virgo collaboration detection of the binary neutron-star merger event, GW170817, has expanded efforts to understand the Equation of State (EoS) of nuclear matter. These measurements provide new constraints on the overall pressure, but do not elucidate its origins, by not distinguishing the contribution to the pressure from symmetry energy which governs much of the internal structure of a neutron star. By combining the neutron star EoS extracted from the GW170817 event and the EoS of symmetric matter from nucleus-nucleus collision experiments, we extract the symmetry pressure, which is the difference in pressure between neutron and nuclear matter over the density region from 1.2 ρ 0 to 4.5 ρ 0. While the uncertainties in the symmetry pressure are large, they can be reduced with new experimental and astrophysical results.