论文标题
限制观察到的旋转速率的毫秒脉冲星的椭圆度
Constraining the ellipticity of millisecond pulsars with observed spin-down rates
论文作者
论文摘要
相对于其自旋轴不对称的旋转中子恒星（NS）可以发出连续的重力波（GW）信号。旋转频率及其分布无线电脉冲星（MSP）和积聚MSP提供了一些GW辐射的证据，而MSP是检测高频GW信号的理想探针。通常认为MSP源于回收过程，其中NS从供体恒星中积聚了材料和角动量。积聚的物质将被固定在NS深层外壳中的压缩磁场的赤道带限制在极性帽区，并产生“磁山”。基于一个假设，即包括PSR J1023+0038在内的三个过渡性MSP的旋转速率是积聚扭矩，螺旋桨扭矩和GW辐射扭矩的组合贡献，我们试图用观察到的旋转率来限制MSP的椭圆率。假设NSS的某些规范参数，估计三个过渡性MSP和十个回溯的椭圆度为$ε=（0.9-23.4）\ times 10^{ - 9} $。三个过渡性MSP的电阻率也被得出在$η=（1.2-15.3）\ times 10^{ - 31}〜\ rm S $的范围内，该\ times 10^{ - 31}〜\ rm s $显示出具有增值率的理想功率法。这些来源发出的GW信号的特征性应变（$ h _ {\ rm c} =（0.6-2.5）\ times10^{ - 27} $）显然超出了aligo的灵敏度范围。我们预计，像爱因斯坦望远镜这样的第三代GW探测器将来可以从这些来源抓住GW信号。
A spinning neutron star (NS) that is asymmetric with respect to its spin axis can emit continuous gravitational wave (GW) signals. The spin frequencies and their distribution of radio millisecond pulsars (MSPs) and accreting MSPs provide some evidences of GW radiation, and MSPs are ideal probes detecting high frequency GW signals. It is generally thought that MSPs originate from the recycled process, in which the NS accretes the material and angular momentum from the donor star. The accreted matter would be confined at the polar cap zone by an equatorial belt of compressed magnetic field fixed in the deep crust of the NS, and yields "magnetic mountain". Based on an assumption that the spin-down rates of three transitional MSPs including PSR J1023+0038 are the combinational contribution of the accretion torque, the propeller torque, and the GW radiation torque, in this work we attempt to constrain the ellipticities of MSPs with observed spin-down rates. Assuming some canonical parameters of NSs, the ellipticities of three transitional MSPs and ten redbacks are estimated to be $ε=(0.9-23.4)\times 10^{-9}$. The electrical resistivities of three transitional MSPs are also derived to be in the range $η=(1.2-15.3)\times 10^{-31}~\rm s$, which display an ideal power law relation with the accretion rate. The characteristic strains ($h_{\rm c}=(0.6-2.5)\times10^{-27}$) of GW signals emitting by these sources are obviously beyond the sensitivity scope of the aLIGO. We expect that the third-generation GW detectors like the Einstein Telescope can seize the GW signals from these sources in the future.
