中子星（NS）的年龄和质量是两条基本线索，使天文学和物理学的其他分支学科能够接触到中子星。这两个参数的准确测定对于理解恒星演化的高级阶段和控制相关过程的物理起着重要作用。在这里，我总结了新的限制的年龄和质量的NS与进化的角度来看。我观察到的P-Pdot人口统计比理论上预测的标准进化通道更多样化。特别是，标准的再循环之后再进行偶极自旋下降，无法以从观测中推导出的速率再现具有更高磁场（B > 4 x 10^{8} G）的毫秒双星的数量。一个适当的列入所产生的限制，从二进制的演化和质量吸积提供了一个更现实的洞察年龄分布。通过分析实现这些限制，我提出了一个“修改”的自旋下降年龄毫秒双星，使估计更接近真实的年龄。最后，我独立地分析了峰值，偏度和截止值的基础质量分布从一个全面的列表中的无线电发射机的安全质量测量是可用的。在双中子星（DNS）和中子星-白矮星（NS-WD）系统中，NS的质量分布分别在1.35 Msun和1.50 Msun处出现明显的峰值。我发现一个质量截止在2 Msun的NS与WD的同伴，这建立了一个坚实的下限的最大质量的NS。
英文摘要：
The ages and masses of neutron stars (NSs) are two fundamental threads that make pulsars accessible to other sub-disciplines of astronomy and physics. A realistic and accurate determination of these two derived parameters play an important role in understanding of advanced stages of stellar evolution and the physics that govern relevant processes. Here I summarize new constraints on the ages and masses of NSs with an evolutionary perspective. I show that the observed P-Pdot demographics is more diverse than what is theoretically predicted for the standard evolutionary channel. In particular, standard recycling followed by dipole spin-down fails to reproduce the population of millisecond pulsars with higher magnetic fields (B > 4 x 10^{8} G) at rates deduced from observations. A proper inclusion of constraints arising from binary evolution and mass accretion offers a more realistic insight into the age distribution. By analytically implementing these constraints, I propose a "modified" spin-down age for millisecond pulsars that gives estimates closer to the true age. Finally, I independently analyze the peak, skewness and cutoff values of the underlying mass distribution from a comprehensive list of radio pulsars for which secure mass measurements are available. The inferred mass distribution shows clear peaks at 1.35 Msun and 1.50 Msun for NSs in double neutron star (DNS) and neutron star-white dwarf (NS-WD) systems respectively. I find a mass cutoff at 2 Msun for NSs with WD companions, which establishes a firm lower bound for the maximum mass of NSs.
Short GRB Host Galaxies. II. A Legacy Sample of Redshifts, Stellar Population Properties, and Implications for their Neutron Star Merger Origins
我们提出了69个短伽玛射线暴（GRB）的宿主星系，代表最大的统一建模的样本日期的恒星星族的性质。使用勘探恒星星族推断代码，我们共同适合每个宿主星系的光度和/或光谱。我们发现一个人口中位数红移$z=0.64^{+0.83}_{-0.32}$（$68\%$信心），包括10个新的或修订的光度红移在$z\gtrsim1$。进一步得到了$t_m=0.8^{+2.71}_{-0.53}$陀螺的质量加权年龄中值，$\log(M_*/M_\odot)=9.69^{+0.75}_{-0.65}$的恒星质量，SFR= $1.44^{+9.37}_{-1.35}M_\odot$ yr $^{-1}$的恒星形成率，$\log(Z_*/Z_\odot)=-0.38^{+0.44}_{-0.42}$的恒星金属丰度，以及$A_V=0.43^{+0.85}_{-0.36}$ ~mag的尘埃衰减（68%置信度）。总的来说，大多数短伽玛暴主机是恒星形成（$\approx84\%$），与小部分的过渡（$\approx6\%$）或静止（$\approx10\%$）;然而，我们观察到一个更大的部分（$\approx40\%$）的静止和过渡主机在$z\lesssim0.25$，与星系演化相称。我们发现，短伽玛射线暴主机填充恒星形成的正常场星系的主要序列，但不包括许多高质量星系，这意味着他们的二进制中子星（BNS）合并的祖先是…
StarHorse results for spectroscopic surveys + Gaia DR3: Chrono-chemical populations in the solar vicinity, the genuine thick disk, and young-alpha rich stars
