The developmental maturity (M) scale using the Star-Wave Test that was independently developed by Yalon and Zion indicates poor learning abilities if the M-scale score is low, which may be caused by developmental dela...The developmental maturity (M) scale using the Star-Wave Test that was independently developed by Yalon and Zion indicates poor learning abilities if the M-scale score is low, which may be caused by developmental delays, such as intellectual disability and learning disorder or organic mental disorder. Furthermore, the distress (D) scale is thought to be influenced by mild neurological disorders, hand coordination problems, and environmental factors. In this study, we conducted a Star-Wave Test on 44 nursery school children in Japan and examined the M scale, the D scale, as well as the level of stress induced by coordination problems and the environment. The t-test was conducted on the M scale and D scale of the group without coordination problems and that with coordination problems, and we found a significant difference at 1% level. From this result, we can confirm the relationship of the M scale and the D scale with Visual and motor maturity.展开更多
随着天文观测数据日益增多,通过数据驱动的方法推断中子星物质的状态方程成为一种可行的方案。本文采用贝叶斯推断和天体物理观测约束相对论平均场(Relativistic Mean Field,RMF)模型,并以此为基础,研究了核状态方程(Equation of State,...随着天文观测数据日益增多,通过数据驱动的方法推断中子星物质的状态方程成为一种可行的方案。本文采用贝叶斯推断和天体物理观测约束相对论平均场(Relativistic Mean Field,RMF)模型,并以此为基础,研究了核状态方程(Equation of State,EOS)和中子星结构。通过分析不同交点密度下与耦合常数密度依赖行为,发现较高的交点密度加强了天体物理观测数据对物态方程的约束,导致大质量中子星的中等密度行为变软,中心能量密度增加。特别地,我们发现包括在大质量中子星核中,声速平方超过共形极限(v_(s)^(2)>1/3)的概率很高。推断的最大中子星质量(M_(max)≥2.5 M⊙)与引力波事件(如GW190814)的解释一致,即其小质量伴星很可能对应于大质量中子星。此外,极端密度下的对称能和压强也表现出交点密度依赖性,符合多信使约束。展开更多
We present a theoretical model for detecting axions from neutron stars in a QCD phase of quark matter. The axions would be produced from a quark-antiquark pair uu¯or dd¯, in loop(s) involving gluons. The chi...We present a theoretical model for detecting axions from neutron stars in a QCD phase of quark matter. The axions would be produced from a quark-antiquark pair uu¯or dd¯, in loop(s) involving gluons. The chiral anomaly of QCD and the spontaneously broken symmetry are invoked to explain the non-conservation of the axion current. From the coupling form factors, the axion emissivities ϵacan be derived, from which fluxes can be determined. We predict a photon flux, which may be detectable by Fermi LAT, and limits on the QCD mass ma. In this model, axions decay to gamma rays in a 2-photon vertex. We may determine the expected fluxes from the theoretical emissivity. The sensitivity curve from the Fermi Large Area Telescope (Fermi LAT) would allow axion mass constraints for neutron stars as low as ma≤10−14eV 95% C.L. Axions could thus be detectable in gamma rays for neutron stars as distant as 100 kpc. A signal from LIGO GWS 170817 could be placed from the NS-NS merger, which gives an upper limit of ma≤10−10eV.展开更多
文摘The developmental maturity (M) scale using the Star-Wave Test that was independently developed by Yalon and Zion indicates poor learning abilities if the M-scale score is low, which may be caused by developmental delays, such as intellectual disability and learning disorder or organic mental disorder. Furthermore, the distress (D) scale is thought to be influenced by mild neurological disorders, hand coordination problems, and environmental factors. In this study, we conducted a Star-Wave Test on 44 nursery school children in Japan and examined the M scale, the D scale, as well as the level of stress induced by coordination problems and the environment. The t-test was conducted on the M scale and D scale of the group without coordination problems and that with coordination problems, and we found a significant difference at 1% level. From this result, we can confirm the relationship of the M scale and the D scale with Visual and motor maturity.
文摘随着天文观测数据日益增多,通过数据驱动的方法推断中子星物质的状态方程成为一种可行的方案。本文采用贝叶斯推断和天体物理观测约束相对论平均场(Relativistic Mean Field,RMF)模型,并以此为基础,研究了核状态方程(Equation of State,EOS)和中子星结构。通过分析不同交点密度下与耦合常数密度依赖行为,发现较高的交点密度加强了天体物理观测数据对物态方程的约束,导致大质量中子星的中等密度行为变软,中心能量密度增加。特别地,我们发现包括在大质量中子星核中,声速平方超过共形极限(v_(s)^(2)>1/3)的概率很高。推断的最大中子星质量(M_(max)≥2.5 M⊙)与引力波事件(如GW190814)的解释一致,即其小质量伴星很可能对应于大质量中子星。此外,极端密度下的对称能和压强也表现出交点密度依赖性,符合多信使约束。
文摘为有效管控民航客机噪声排放对机场及附近城市等关键空间位置点的影响,强化飞行程序设计对四型机场建设支撑作用。以单事件综合噪声模型(Integrated Noise Model,INM)为基础,考虑飞行各阶段航空器性能和飞行程序设计规范,建立噪声分布与波状趋势分析模型(Noise Distribution and Wave Trend Analysis Model,NWA),利用以航空器基础资料(Base of Aircraft Data,BADA)为基础的BADA航空器性能模型实现航迹仿真,获得基于航迹的噪声值与波状趋势量化计算结果,完成噪声等值线图绘制。计算结果表明:采用低于70分贝圈与机场所需性能导航(Required Navigation Performance,RNP)进场程序保护区宽度作为航迹调整值,其噪声分布与波状趋势的影响范围变化较明显,关键空间位置点受噪声影响程度与时长均大幅降低。在NWA可靠性方面,其结果具有符合飞行性能特征,计算精度较高等优势。
文摘We present a theoretical model for detecting axions from neutron stars in a QCD phase of quark matter. The axions would be produced from a quark-antiquark pair uu¯or dd¯, in loop(s) involving gluons. The chiral anomaly of QCD and the spontaneously broken symmetry are invoked to explain the non-conservation of the axion current. From the coupling form factors, the axion emissivities ϵacan be derived, from which fluxes can be determined. We predict a photon flux, which may be detectable by Fermi LAT, and limits on the QCD mass ma. In this model, axions decay to gamma rays in a 2-photon vertex. We may determine the expected fluxes from the theoretical emissivity. The sensitivity curve from the Fermi Large Area Telescope (Fermi LAT) would allow axion mass constraints for neutron stars as low as ma≤10−14eV 95% C.L. Axions could thus be detectable in gamma rays for neutron stars as distant as 100 kpc. A signal from LIGO GWS 170817 could be placed from the NS-NS merger, which gives an upper limit of ma≤10−10eV.
