A NEW CORRELATION WITH LOWER KILOHERTZ QUASI-PERIODIC OSCILLATION FREQUENCY IN THE ENSEMBLE OF LOW-MASS X-RAY BINARIES
A NEW CORRELATION WITH LOWER KILOHERTZ QUASI-PERIODIC OSCILLATION FREQUENCY IN THE ENSEMBLE OF LOW-MASS X-RAY BINARIES
复制标题
低质量X射线双星系综中低千赫准周期振荡频率的新关联
DOI：
10.3847/0004-637x/831/1/25
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
Onur Çatmabacak
中科院分区：
文献类型：
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作者：
M. Hakan Erkut;Şİvan Duran;Önder Çatmabacak;Onur Çatmabacak
我们研究了中子星低质量 X 射线双星系统中千赫兹准周期振荡 (kHz QPO) 频率对吸积相关参数的依赖性。根据中子星表面的质量吸积率 和磁场强度 B，我们发现较低 kHz QPO 频率和 之间存在相关性。这种相关性在 Z 源和环礁源的当前系综中成立，因此可以解释同一系综中 kHz QPO 频率和 X 射线光度之间缺乏相关性。整个相关过程中较低 kHz QPO 频率的平均运行可以通过源数据的幂律拟合来描述。然而，简单的幂律无法描述单个源的频率分布。另一方面，拟合频率数据的模型函数可以解释在单个源以及源集合的情况下观察到的较低 kHz QPO 频率的分布。模型函数取决于基本长度尺度，例如磁层半径和边界区域的径向宽度，这两者都预计会随着确定 QPO 频率而变化。除了修改长度尺度并因此修改 QPO 频率之外，足够大的变化也可能导致不同的吸积机制，其特征在于 Z 和环礁相位。
We study the dependence of kilohertz quasi-periodic oscillation (kHz QPO) frequency on accretion-related parameters in the ensemble of neutron-star low-mass X-ray binaries. Based on the mass accretion rate, , and the magnetic field strength, B, on the surface of the neutron star, we find a correlation between the lower kHz QPO frequency and . The correlation holds in the current ensemble of Z and atoll sources and therefore can explain the lack of correlation between the kHz QPO frequency and X-ray luminosity in the same ensemble. The average run of lower kHz QPO frequencies throughout the correlation can be described by a power-law fit to source data. The simple power law, however, cannot describe the frequency distribution in an individual source. The model function fit to frequency data, on the other hand, can account for the observed distribution of lower kHz QPO frequencies in the case of individual sources as well as the ensemble of sources. The model function depends on the basic length scales, such as the magnetospheric radius and the radial width of the boundary region, both of which are expected to vary with to determine the QPO frequencies. In addition to modifying the length scales, and hence the QPO frequencies, the variation in , being sufficiently large, may also lead to distinct accretion regimes, which would be characterized by Z and atoll phases.
影响因子：
4.8
作者：
J. Binney;B. Burnett;G. Kordopatis;P. McMillan;Sanjib Sharma;T. Zwitter;O. Bienaymé;J. Bland-Hawthorn-J.
通讯作者：
J. Binney;B. Burnett;G. Kordopatis;P. McMillan;Sanjib Sharma;T. Zwitter;O. Bienaymé;J. Bland-Hawthorn-J.