论文标题
双中性星系J1829+2456的精确质量测量值
Precise mass measurements for the double neutron star system J1829+2456
论文作者
论文摘要
PSR J1829+2456是一个相对论二进制系统中的无线电脉冲星，带有另一个中子星。它的旋转周期为41毫秒，偏心偏心（$ e = 0.14 $）28小时轨道。我们一直使用Arecibo射电望远镜进行观察，现在测量了该系统的单个中子星质量。 Pulsar and Companion块为$ 1.306 \，\ pm \，0.007 \，m _ {\ odot} $和$ 1.299 \，\，\ pm \，0.007 \，0.007 \，m _ {\ odot} $（2 $σ$ - 95％的信心，除非分别说明）。我们还测量了该系统的适当运动，并用它来估计49 $^{+77} _ { - 30} $ km s $ s $^{ - 1} $相对于本地静止标准的空间速度。该系统中伴随质量，空间速度和轨道偏心的相对较低的值使其与其他双中性恒星系统相似，在该系统中，第二形式的中子恒星被认为是在低键，低质量，对称的超级诺娃中形成的。
PSR J1829+2456 is a radio pulsar in a relativistic binary system with another neutron star. It has a rotational period of 41 ms and a mildly eccentric ($e = 0.14$) 28-hr orbit. We have continued its observations with the Arecibo radio telescope and have now measured the individual neutron star masses of this system. The pulsar and companion masses are $1.306\,\pm\,0.007\,M_{\odot}$ and $1.299\,\pm\,0.007\,M_{\odot}$ (2$σ$ - 95% confidence, unless stated otherwise), respectively. We have also measured the proper motion for this system and used it to estimate a space velocity of 49$^{+77}_{-30}$ km s$^{-1}$ with respect to the local standard of rest. The relatively low values for companion mass, space velocity and orbital eccentricity in this system make it similar to other double neutron star systems in which the second-formed neutron star is thought to have formed in a low-kick, low mass-loss, symmetric supernova.
