THE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS
THE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS
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DOI：
10.3847/0004-637x/820/1/28
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发表时间：
2015-05
期刊：
影响因子：
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通讯作者：
F. Özel;D. Psaltis;T. Güver;G. Baym;C. Heinke;S. Guillot
中科院分区：
文献类型：
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作者：
F. Özel;D. Psaltis;T. Güver;G. Baym;C. Heinke;S. Guillot
我们提出了一个全面的研究光谱半径测量12颗中子星获得在热核爆发或在静止。我们首次在视角尺寸、爱丁顿通量和距离的测量、星际介质的组成以及x射线探测器的通量校准中纳入了大量的系统不确定性。我们还考虑到最近关于旋转对中子星半径的影响、大气对表面光谱的影响以及爱丁顿临界通量的相对论修正的理论计算结果。我们利用贝叶斯统计框架从光谱测量中得到中子星半径，并从半径测量中推断出中子星的状态方程。将这些结果与核饱和密度附近的实验结果和~ 2 M⊙？我们对中子星在≈2 - 8 ?之间的状态方程的性质施加了强有力的定量约束。>乘以核饱和密度。我们发现在M = 1.5 M⊙,？>首选状态方程预测半径在10.1到11.1公里之间。当在基于相互作用核子的高密度状态方程中解释压力约束时，我们的结果表明三体相互作用势的贡献相对较弱。
We present a comprehensive study of spectroscopic radius measurements of twelve neutron stars obtained during thermonuclear bursts or in quiescence. We incorporate, for the first time, a large number of systematic uncertainties in the measurement of the apparent angular sizes, Eddington fluxes, and distances, in the composition of the interstellar medium, and in the flux calibration of X-ray detectors. We also take into account the results of recent theoretical calculations of rotational effects on neutron star radii, of atmospheric effects on surface spectra, and of relativistic corrections to the Eddington critical flux. We employ Bayesian statistical frameworks to obtain neutron star radii from the spectroscopic measurements as well as to infer the equation of state from the radius measurements. Combining these with the results of experiments in the vicinity of nuclear saturation density and the observations of ∼ 2 M ⊙ ?> neutron stars, we place strong and quantitative constraints on the properties of the equation of state between ≈ 2 – 8 ?> times the nuclear saturation density. We find that around M = 1.5 M ⊙ , ?> the preferred equation of state predicts radii between 10.1 and 11.1 km. When interpreting the pressure constraints in the context of high density equations of state based on interacting nucleons, our results suggest a relatively weak contribution of the three-body interaction potential.