论文标题
通过重力波和无线电观察，对人口I/II中子星空孔二元二元形成的限制
Constraints on Population I/II neutron star-black hole binary formation by gravitational wave and radio observations
论文作者
论文摘要
在Ligo/Pirgo O3B运行中发现的两个中子星（NS） - 黑孔（BH）二进制文件，GW200105和GW200115的BH质量较小，为6--9 \，$ M _ {\ odot} $，与人口I和II的起源是一致的。我们的人口合成模拟使用$ 10^6 $ IS i和ii二进制文件具有适当的初始参数的二进制质量，事件速率，无线电脉冲星（PSR）（PSR）和BH二进制文件均保持一致。尤其是，我们发现了GW200105和GW200115的可能祖细胞，它们以红移$ z = 0.15 $和$ z = 1.6 $形成，二进制质量为$（3400万_ {\ odot}，\，\，92m _ {\ odot}）分别为106m _ {\ odot}）$。这些二进制文件的最终质量为$（685万_ {\ odot}，\，\，2.14m _ {\ odot}）$和$（604万_ {\ odot}，\，\，131m _ {\ odot} $（9.0 _ { - 1.7}^{+1.7} m _ {\ odot}，\，\，1.91 _ { - 0.24}^{+0.33} m _ {\ odot}）$ gw200105和gw200105和$（5.9 _ { - 2.5}^{+2.0} m _ {\ odot}，\，\，1.44 _ { - 0.29}^{+0.85} m _ {\ odot}）$分别of GW200115的$。我们还估计，SKA将观察到我们星系中的2.68-19.7 PSR-BH二进制文件。在我们的银河系中，可以在未来的SKA时代确认NS-BH的存在。使用GW对NS-BH合并的观察以及将来对PSR-BH的无线电观察，我们可以在NS-BH组形成过程中获得更严重的限制。
Two neutron star (NS)-black hole (BH) binaries, GW200105 and GW200115 found in the LIGO/Virgo O3b run have smaller BH mass of 6--9\,$M_{\odot}$ which is consistent with Population I and II origin. Our population synthesis simulations using $10^6$ Population I and II binaries with appropriate initial parameters show consistent binary mass, event rate, and no detection of radio pulsar (PSR) and BH binaries in our galaxy so far. Especially, we found possible progenitors of GW200105 and GW200115 which were formed at redshift $z=0.15$ and $z=1.6$ with binary mass of $(34M_{\odot},\, 9.2M_{\odot})$ and $(23.7M_{\odot},\, 10.6M_{\odot})$, respectively. The final masses of these binaries are $(6.85M_{\odot},\,2.14M_{\odot})$ and $(6.04M_{\odot},\,1.31M_{\odot})$ which look like $(9.0_{-1.7}^{+1.7}M_{\odot},\, 1.91_{-0.24}^{+0.33}M_{\odot})$ of GW200105 and $(5.9_{-2.5}^{+2.0}M_{\odot},\,1.44_{-0.29}^{+0.85}M_{\odot})$ of GW200115, respectively. We also estimate that 2.68-19.7 PSR-BH binaries in our galaxy will be observed by SKA. The existence of NS-BHs in our galaxy can be confirmed in future SKA era. Using the GW observation of NS-BH mergers and the radio observation of PSR-BHs in future, we can get more severe constraints on the NS-BH formation process.
