论文标题
按照银河系人口所暗示的合并双中子星的质量比
Mass Ratios of Merging Double Neutron Stars as Implied by the Milky Way Population
论文作者
论文摘要
在七个已知的双中性恒星（DNS）中，它们以银河系的测量质量在笨拙的时间内合并，除了一个外，所有质量比$ q $都接近统一。最近，DNS J1913 $+$ 1102中三个雄性后参数的精确度量限制了该系统的明显非统一质量比为0.78 $ \ pm $ 0.03。可以得出结论，在重力波观测器检测到的七个（14 \％）DNS合并中，大约有1个与统一的质量比明显不同。但是J1913 $+$ 1102的合并时间相对较长，为470 Myr。我们表明，当考虑到合并时间和观察性偏见时，银河系DNSS的种群暗示所有合并DNSS中的$ \ simeq98 \％$将具有$ Q> $> $ 0.9。 We then apply two separate fitting formulas informed by 3D hydrodynamic simulations of DNS mergers to our results on Galactic DNS masses, finding that either $\simeq$0.004 ${M_{\odot}}$ or $\simeq$0.010 ${M_{\odot}}$ of material will be ejected at merger, depending on which formula is 用过的。这些弹射质量对电磁对应物的峰值辐射仪具有影响（我们认为这是$ \ sim $ 10 $^{41} $ erg s $^{ - 1} $，以及$ r $ $ - $ -R $ -Process的丰富。
Of the seven known double neutron stars (DNS) with precisely measure masses in the Milky Way that will merge within a Hubble time, all but one has a mass ratio, $q$, close to unity. Recently, precise measurements of three post-Keplerian parameters in the DNS J1913$+$1102 constrain this system to have a significantly non-unity mass ratio of 0.78$\pm$0.03. One may be tempted to conclude that approximately one out of seven (14\%) DNS mergers detected by gravitational wave observatories will have mass ratios significantly different from unity. However J1913$+$1102 has a relatively long merger time of 470 Myr. We show that when merger times and observational biases are taken into account, the population of Galactic DNSs imply that $\simeq98\%$ of all merging DNSs will have $q>$0.9. We then apply two separate fitting formulas informed by 3D hydrodynamic simulations of DNS mergers to our results on Galactic DNS masses, finding that either $\simeq$0.004 ${M_{\odot}}$ or $\simeq$0.010 ${M_{\odot}}$ of material will be ejected at merger, depending on which formula is used. These ejecta masses have implications for both the peak bolometric luminosities of electromagnetic counterparts (which we find to be $\sim$10$^{41}$ erg s$^{-1}$) as well as the $r$-process enrichment of the Milky Way.
