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X-ray timing properties of Cygnus X-1 and Cygnus X-2.

机译:天鹅座X-1和天鹅座X-2的X射线定时特性。

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摘要

Cygnus X-1 and Cygnus X-2 are X-ray sources which are believed to be a black hole and a neutron star, respectively.;We investigate the variability of Cygnus X-1 in the context of shot noise models, and employ a peak detection algorithm to select individual shots. The detected shots are fit to several model templates. The fit shot parameters are found to be distributed.;The cross spectrum of light curves from Cygnus X-1 in different energy bands is studied. Large, frequency dependent time lags are observed, along with high coherence. The high coherence implies that the transfer function between low and high energy variability is uniform. This implies that, if the lags are due to Compton scattering, variations in the seed intensity must originate in a region much smaller than the Comptonizing medium. The frequency dependence of the lags implies that, if they are due to Comptonization, the Comptonizing medium is nonuniform.;The uniformity of the transfer function implies that the observed distribution of shot widths cannot have been acquired through Compton scattering.;The energy spectrum of the radiation reaching us from Cygnus X-1 is found to fluctuate at the shortest timescales observable. This implies rapid changes in the geometry or temperature of some portions of the system, possibly due to dynamical instabilities of the system.;The high counting rates and temporal resolution of the Rossi X-ray Timing Explorer allow more detailed investigation of the Horizontal Branch Oscillations (HBO) in Cygnus X-2 than has been possible previously, including observation of a second harmonic. The relations of the frequencies and widths of these peaks are investigated in order to shed light on their origin and thus the conditions in the region of their formation. The observations support the Magnetospheric Beat Frequency Modulated Accretion model for the origin of the HBO. The data indicate that neither rapid variation in the frequency of, nor short lifetime of, a locally coherent oscillation is sufficient to explain the broadening alone. This argues that the width is due to the simultaneous presence of multiple frequencies, or limitation of the amplitude of oscillations through some nonlinear effect.
机译:天鹅座X-1和天鹅座X-2是分别被认为是黑洞和中子星的X射线源;;我们在散粒噪声模型的背景下研究了天鹅座X-1的变异性,并采用峰值检测算法选择单个镜头。检测到的镜头适合多个模型模板。发现适合的射击参数是分布的;研究了天鹅座X-1在不同能带的光曲线的交叉光谱。观察到较大的,与频率相关的时滞以及高相干性。高相干性意味着低和高能量变异性之间的传递函数是均匀的。这意味着,如果滞后归因于康普顿散射,则种子强度的变化必须起源于比康普顿化介质小得多的区域。滞后的频率依赖性意味着,如果它们是由于康普顿化引起的,则康普顿化介质是不均匀的;传递函数的均匀性意味着不能通过康普顿散射获得观测到的散布宽度的分布。从天鹅座X-1到达我们的辐射被发现在可观察到的最短时间范围内波动。这意味着可能由于系统的动态不稳定性而导致系统某些部分的几何形状或温度发生快速变化。; Rossi X射线定时资源管理器的高计数率和时间分辨率允许更详细地研究水平分支振荡Cygnus X-2中的“ HBO”(HBO)比以前可能的更高,包括观察到二次谐波。研究了这些峰的频率和宽度之间的关系,以阐明其起源以及由此形成区域的条件。这些观测结果支持了HBO起源的磁层拍频调制吸积模型。数据表明,局部相干振荡频率的快速变化或较短的寿命都不足以单独解释这种扩展。这表明宽度是由于同时存在多个频率,或者是由于某种非线性效应限制了振荡幅度。

著录项

  • 作者

    Focke, Warren Bosworth.;

  • 作者单位

    University of Maryland, College Park.;

  • 授予单位 University of Maryland, College Park.;
  • 学科 Physics Astronomy and Astrophysics.
  • 学位 Ph.D.
  • 年度 1998
  • 页码 166 p.
  • 总页数 166
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

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