The ultraluminous X-ray source NuSTAR J095551+6940.8: a magnetar in a high-mass X-ray binary
The ultraluminous X-ray source NuSTAR J095551+6940.8: a magnetar in a high-mass X-ray binary
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DOI：
10.1093/mnrasl/slu199
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发表时间：
2014-10
影响因子：
4.8
通讯作者：
K. Ekşi;I. C. Andaç;S. Çıkıntoğlu;A. A. Gençali-A.;C. Güngör;F. Öztekin
中科院分区：
文献类型：
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作者：
K. Ekşi;I. C. Andaç;S. Çıkıntoğlu;A. A. Gençali-A.;C. Güngör;F. Öztekin
Bachetti等人最近在M82中探测到来自超亮X射线源（ULX）努斯塔J 095551 +6940.8的脉动，表明该物体是高质量X射线双星（HMXB）系统中的吸积中子星星。该天体的超爱丁顿光度意味着磁场足够强以抑制散射截面，除非它的光束是在一个有利的角度。我们证明了脉冲星的力矩平衡条件表明中子星星的偶极磁场为6.7 × 10^{13}$ G，比Bachetti等人估计的高两个数量级，并进一步指出，更强的磁场很可能存在于更高的多极中。这支持了最近的观点，即如果磁场在过渡过程中衰减一个数量级，磁星就会从HMXB下降。
The recent detection of pulsations from the ultra luminous X-ray source (ULX) NuSTAR J095551+6940.8 in M82 by Bachetti et al. indicates that the object is an accreting neutron star in a high mass X-ray binary (HMXB) system. The super-Eddington luminosity of the object implies that the magnetic field is sufficiently strong to suppress the scattering cross-section unless its beam is viewed at a favourable angle. We show that the torque equilibrium condition for the pulsar indicates the dipole magnetic field of the neutron star is $6.7 \times 10^{13}$ G, two orders of magnitude higher than that estimated by Bachetti et al., and further point to the possibility that even stronger magnetic fields could well be in the higher multipoles. This supports the recent view that magnetars descent from HMXBs if the magnetic field decays an order of magnitude during the process of transition.