论文标题
积聚X射线脉冲星的极化。 ii。大力神X-1
Polarisation of Accreting X-ray Pulsars. II. Hercules X-1
论文作者
论文摘要
我们采用了新模型来积聚X射线脉冲星的极化发射，以描述发光的X射线脉冲星赫拉克勒斯X-1的发射。与以前的工作相反，我们的模型可以独立于光谱形成来预测极化参数，并考虑了增生柱的结构和动力学，以及由于一般相对论和量子电动力学而引起的对传播的其他影响。我们发现，我们的模型可以描述观察到的脉冲分数和主峰的脉冲形状，以及与相位相结合线的调制。我们选择两个几何形状，假设在磁极处有一个或两个列，可以描述脉冲形状和回旋子调制的当前观察结果。这两种模型都预测，在$ 1-10 $ keV范围内的60至80 \％之间的高极化分数（均为相位和能量依赖性），并且与强度相同的阶段达到峰值。极化分数和极化角的相位和能量依赖性可以帮助识别不同几何形状。
We employ our new model for the polarised emission of accreting X-ray pulsars to describe the emission from the luminous X-ray pulsar Hercules X-1. In contrast with previous works, our model predicts the polarisation parameters independently of spectral formation, and considers the structure and dynamics of the accretion column, as well as the additional effects on propagation due to general relativity and quantum electrodynamics. We find that our model can describe the observed pulse fraction and the pulse shape of the main peak, as well as the modulation of the cyclotron line with phase. We pick two geometries, assuming a single accretion column or two columns at the magnetic poles, that can describe current observations of pulse shape and cyclotron modulation with phase. Both models predict a high polarisation fraction, between 60 and 80\% in the $1-10$ keV range, that is phase- and energy-dependent, and that peaks at the same phase as the intensity. The phase and energy dependence of the polarisation fraction and of the polarisation angle can help discern between the different geometries.
