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Staring at 4U 1909+07 with Suzaku

机译:朱雀凝视着4U 1909 + 07

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摘要

We present an analysis of the neutron star high mass X-ray binary (HMXB) 4U 1909+07 mainly based on Suzaku data. We extend the pulse period evolution, which behaves in a random-walk like manner, indicative of direct wind accretion. Studying the spectral properties of 4U 1909+07 between 0.5 to 90 keV we find that a power-law with an exponential cutoff can describe the data well, when additionally allowing for a blackbody or a partially covering absorber at low energies.ududWe find no evidence for a cyclotron resonant scattering feature (CRSF), a feature seen in many other neutron star HMXBs sources. By performing pulse phase resolved spectroscopy we investigate the origin of the strong energy dependence of the pulse profile, which evolves from a broad two-peak profile at low energies to a profile with a single, narrow peak at energies above 20 keV. Our data show that it is very likely that a higher folding energy in the high energy peak is responsible for this behavior. This in turn leads to the assumption that we observe the two magnetic poles and their respective accretion columns at different phases, and that these accretion columns have slightly different physical conditions.
机译:我们主要基于朱雀学数据,对中子星高质量X射线双星(HMXB)4U 1909 + 07进行分析。我们扩展了脉冲周期的演变,这种变化以随机游走的方式表现,表明直接的风积聚。通过研究4U 1909 + 07在0.5至90 keV之间的光谱特性,我们发现具有指数截止值的幂律可以很好地描述数据,同时还允许使用低能量的黑体或部分覆盖的吸收体。 ud udWe找不到回旋加速器共振散射特征(CRSF)的证据,回旋加速器共振散射特征(CRSF)是许多其他中子星HMXBs源中所见的特征。通过执行脉冲相位分辨光谱法,我们研究了脉冲轮廓的强能量依赖性的起源,其从低能量的宽两峰轮廓演变为在20 keV以上的能量具有单个窄峰的轮廓。我们的数据表明,很可能是高能峰中较高的折叠能导致了此行为。这进而导致一个假设,即我们在不同相位观察两个磁极及其各自的吸积柱,并且这些吸积柱的物理条件略有不同。

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