论文标题
部分可观测时空混沌系统的无模型预测
Formation of black widows through ultra-compact X-ray binaries with He star companions
论文作者
论文摘要
黑寡妇（BWS）是一种带有伴侣群体的千分之一的脉冲星（MSP）$ M_2 $ \ lyseSim 0.05 \，\ rm m_ \ odot $，可用于研究增生历史和脉冲星的辐射，以及脉搏的辐射以及隔离的MSP的启发。最近的观察结果表明，BWS有两种子类型。一个是带有$ M_2 $ $ \ sim $ 0.01-0.05 \，\ rm m_ \ odot $的BWS，而另一个则带有$ M_2 $ $ \ sillesim 0.01 \，\ rm m_ \ odot $。但是，后者的起源仍然高度不确定。在本文中，我们通过Ultra-Compact X射线二进制文件（UCXBS）与$ M_2 $ $ $ $ $ $ $ \ LYSSIM 0.01 \，\ rm m_ \ odot $一起使用He Star Companions，其中中立星（NS）Accretes Accretes材料来自He He a He ta He ta He take Roche-lobe溢出。通过考虑不同的质量和蒸发效率，具有用于恒星天体物理学实验（MESA）实验的恒星演化代码模块（MESA），我们进化了一系列的NS+He Star系统，这些系统可以进行UCXB阶段。我们发现，该频道可以解释BWS在Hubble时间内使用$ M_2 $ $ \ lyssim 0.01 \，\ rm m_ \ odot $的形成，尤其是三个广泛研究的BWS，即PSRS J1719-1438，J2322-2650和J1311-2650和J1311--3430。我们还发现，X射线辐照反馈不会影响蒸发过程的进化轨道。我们的模拟表明，与He Star同伴的UCXB通道是孤立的MSP的潜在祖细胞，并且具有$ M_2 $ $ $ \ Lessim 0.01 \，\ rm m_ \ odot $的BW的起源与另一个子类型的BWS不同。此外，目前的工作表明，具有$ M_2 $ $ $ \ lyssim 0.01 \，\ rm m_ \ odot $的BWS可能不会由Redback Systems生产。
Black widows (BWs) are a type of eclipsing millisecond pulsars (MSPs) with companion masses $M_2$ $\lesssim 0.05\,\rm M_\odot$, which can be used to study the accretion history and the radiation of pulsars, as well as the origin of isolated MSPs. Recent observations indicate that there are two sub-types of BWs. One is the BWs with $M_2$ $\sim$ $0.01-0.05\,\rm M_\odot$, whereas another with $M_2$ $\lesssim 0.01\,\rm M_\odot$. However, the origin of the latter is still highly uncertain. In this paper, we investigated the formation of BWs with $M_2$ $\lesssim 0.01\,\rm M_\odot$ through ultra-compact X-ray binaries (UCXBs) with He star companions, in which a neutron star (NS) accretes material from a He star through Roche-lobe overflow. By considering different He star masses and evaporation efficiencies with the stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA), we evolved a series of NS+He star systems that can undergo UCXB stage. We found that this channel can explain the formation of BWs with $M_2$ $\lesssim 0.01\,\rm M_\odot$ within the Hubble time, especially three widely studied BWs, i.e. PSRs J1719-1438, J2322-2650 and J1311-3430. We also found that X-ray irradiation feedback does not affect the evolutionary tracks of evaporation process. Our simulations indicate that the UCXB channel with He star companions are the potential progenitors of isolated MSPs, and that the origin of BWs with $M_2$ $\lesssim 0.01\,\rm M_\odot$ is different with another sub-type of BWs. In addition, the present work suggests that the BWs with $M_2$ $\lesssim 0.01\,\rm M_\odot$ may not be produced by redback systems.
