Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
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DOI：
10.1038/s41550-020-1014-6
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发表时间：
2020-03-09
期刊：
影响因子：
14.1
通讯作者：
Reddy, Sanjay
中科院分区：
文献类型：
--
作者：
Capano, Collin D.;Tews, Ingo;Reddy, Sanjay
中子星的性质是由它们所含物质的性质决定的。这些特性可以通过测量恒星的大小来限制。我们通过结合双中子星合并GW170817的多源观测和最好地解释状态方程中密度相关不确定性的核理论，获得了对中子星半径的严格约束。我们构造了受手征有效场理论约束的状态方程，并利用引力波观测对其进行了边际化。结合合并残余物的电磁观测，我们发现一颗1.4M圆点中子星的半径为R1.4M圆点=11.0-0.6+0.9公里(90%可信区间)。利用这个约束，我们证明了在中子星-黑洞合并中，中子星不太可能被破坏；因此，这样的事件不会产生可观察到的电磁辐射。
The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star's size. We obtain stringent constraints on neutron-star radii by combining multimessenger observations of the binary neutron-star merger GW170817 with nuclear theory that best accounts for density-dependent uncertainties in the equation of state. We construct equations of state constrained by chiral effective field theory and marginalize over these using the gravitational-wave observations. Combining this with the electromagnetic observations of the merger remnant that imply the presence of a short-lived hypermassive neutron star, we find that the radius of a 1.4 M-circle dot neutron star is R1.4M circle dot=11.0-0.6+0.9km (90% credible interval). Using this constraint, we show that neutron stars are unlikely to be disrupted in neutron star-black hole mergers; subsequently, such events will not produce observable electromagnetic emission.