论文标题
伽玛射线二进制LS I +61°303是否有磁铁？
Does the gamma-ray binary LS I +61°303 harbor a magnetar?
论文作者
论文摘要
高质量X射线二进制LS I +61°303也因TEV光子能量经常出现而作为伽马射线二进制分类。该系统过去释放了两种软γ耀斑，这表明对紧凑型初级的磁性解释。在发现瞬态无线电脉冲之后，该推断最近在系统的某些轨道阶段中发现了巨大的吸引力，因为测量的旋转和暂定旋转速率意味着$ b_p \ gtrsim 10^{14} \，\ mbox {g} $ b_p \ gtrsim 10^{14} \} $ if star a Star Is via nage dipole dipole dipole dipole。在本文中，我们通过分析可用数据的兼容性与系统的积分动力学，自旋进化，年龄限制，伽马射线排放和无线电脉冲星的激活来仔细检查磁场估计值。我们发现，除非强大的螺旋桨扭矩正在运行，否则在理论上很难和解中子恒星的年龄和自旋进化。这种扭矩也可能导致大部分甚至最大允许的旋转，可能会削弱推断的磁场的数量级。
The high-mass X-ray binary LS I +61°303 is also cataloged as a gamma-ray binary as a result of frequent outbursts at TeV photon energies. The system has released two soft-gamma flares in the past, suggesting a magnetar interpretation for the compact primary. This inference has recently gained significant traction following the discovery of transient radio pulses, detected in some orbital phases from the system, as the measured rotation and tentative spin-down rates imply a polar magnetic field strength of $B_p \gtrsim 10^{14}\,\mbox{G}$ if the star is decelerating via magnetic dipole braking. In this paper, we scrutinize magnetic field estimates for the primary in LS I +61°303 by analyzing the compatibility of available data with the system's accretion dynamics, spin evolution, age limits, gamma-ray emissions, and radio pulsar activation. We find that the neutron star's age and spin evolution are theoretically difficult to reconcile unless a strong propeller torque is in operation. This torque could be responsible for the bulk of even the maximum allowed spin-down, potentially weakening the inferred magnetic field by more than an order of magnitude.
