论文标题
在超大型X射线源NGC 300 ULX1中的中子星的质量和磁场上
On the Mass and Magnetic Field of the Neutron Star in the Ultraluminous X-Ray Source NGC 300 ULX1
论文作者
论文摘要
在大多数超X射线源（ULX）中，积分紧凑的物体可能是中子星而不是黑洞，这是由于最近发现来自邻近星系中的某些源的周期性脉动所建议的，而在我们自己的星系中发现了一个迄今已发现的ULX。作为ULX家族的成员，NGC 300 ULX1是一种新的脉动ULX（PULX），与其他PULX相比，速率高得多。在本文中，通过使用观察到的X-READ的X-Ray估算了X-Ray的X-Ray估算，从NGC 300 ULX1的脉冲X射线光谱中检测到的中性恒星表面上的磁场强度是从NGC 300 ULX1的脉冲X射线光谱中检测到的中子能吸收线的强度和中子星质量和光束分数的合理范围的。我们的分析有利于质子回旋共振散射作为一种可行的机制，可以说明观察到的回旋通能量和高旋转速率，前提是吸收线是在中子恒星表面附近产生的。
The accreting compact objects in most of ultraluminous X-ray sources (ULXs) are likely to be neutron stars rather than black holes as suggested by the recent detection of periodic pulsations from some of these sources located in neighboring galaxies and one ULX that has hitherto been discovered in our own galaxy. As a member of the ULX family, NGC 300 ULX1 is a new pulsating ULX (PULX) spinning up at substantially high rates compared with other PULXs. In this paper, the strength of the magnetic field on the surface of the neutron star is inferred from the energy of the cyclotron absorption line detected in the pulsed X-ray spectrum of NGC 300 ULX1 and the plausible ranges for the neutron-star mass and beaming fraction are estimated using the observed spin period and period derivative of the pulsar and the measured X-ray flux of the source. Our analysis favors proton cyclotron resonance scattering as a viable mechanism to account for both the observed cyclotron energy and high spin-up rates provided that the absorption line is generated close to the surface of the neutron star.
