Exploring the accretion-induced evolution of the spin period and magnetic field strength of Be/X-ray Pulsars
Exploring the accretion-induced evolution of the spin period and magnetic field strength of Be/X-ray Pulsars
复制标题
探索 Be/X 射线脉冲星自旋周期和磁场强度的吸积诱发演化
DOI：
10.1007/s10509-020-03841-2
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发表时间：
2020
影响因子：
1.9
通讯作者：
Zhang Jian-Wei
中科院分区：
文献类型：
--
作者：
Ye Chang-Qing;Wang De-Hua;Zhang Cheng-Min;Zhang Jian-Wei
基于检测到的自旋周期 () 和通过回旋共振散射特征推断出的磁场强度 ()，我们分析了 Be/X 射线脉冲星 (BeXP) 的特性。我们发现BeXPs的分布呈现出ats分离的双峰特征，其中BeXPs的平均自旋周期（s）比源的平均自旋周期（s）大大约一个数量级。同时，长周期BeXPs（G）的平均磁场强度比短周期源（G）高出0.5倍。我们试图用吸积诱发演化过程来解释这些现象，发现对于初始磁场强度为G的中子星（NS），当它吸积伴星时，它的自转周期可以缩短，而其磁场强度衰减很小。此外，当NS吸积物质时，其自旋周期可以缩短至s，而其磁场强度则衰减一半。最后，我们还注意到，随着Be/X射线双星吸积过程的继续，当其NS吸积物质时，它有可能演化为双中子星。
Based on the detected spin periods () and inferred magnetic field strengths () by the cyclotron resonance scattering features, we analyze theproperties of Be/X-ray Pulsars (BeXPs). We find that thedistribution of BeXPs exhibits a bimodal feature separated ats, where the average spin period of the BeXPs withs (s) is larger than that of the sources withs (s) by about one magnitude of order. Meanwhile, the average magnetic field strength of the long period BeXPs (G) is higher than that of the short period sources (G) by a factor of. We try to explain these phenomena by the accretion-induced evolution process, and find that for the neutron star (NS) with the initial magnetic field strength ofG, when it accretes aboutcompanion matter, its spin period can shorten froms tos, while its magnetic field strength decays little. Furthermore, when the NS accretes aboutmatter, its spin period can shorten tos, while its magnetic field strength decays by half. Finally, we also notice that as the continuing of the accretion process in Be/X-ray binary, when its NS accretes aboutmater, it has the possibility to evolve to the double neutron star.