GX 339—4: the distance, state transitions, hysteresis and spectral correlations
GX 339—4: the distance, state transitions, hysteresis and spectral correlations
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DOI：
10.1111/j.1365-2966.2004.07830.x
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发表时间：
2004-02
影响因子：
4.8
通讯作者：
A. Zdziarski;M. Gierliński;J. Mikołajewska;G. Wardziński;David M. Smith;B. A. Harmon;S. Kitamoto
中科院分区：
文献类型：
--
作者：
A. Zdziarski;M. Gierliński;J. Mikołajewska;G. Wardziński;David M. Smith;B. A. Harmon;S. Kitamoto
我们研究了GX 339-4的X射线和变异性以及距离。我们推导出的距离> 7千秒差距，根据最近确定的二进制参数。我们研究了Ginga上的ASM、CGRO上的BatSE以及RXTE上的ASM、PCA和HEXTE的数据。从1987年到2004年，GX 339-4经历了15次爆发，并经历了所有已知的黑洞双星状态。首次给出了2004年爆发初始硬态的主成分分析数据。然后，我们研究colourcolour和颜色通量的相关性。在硬态下，1.5-5和3-12 keV的光谱斜率之间存在很强的负相关关系，我们用盘光子的热康普顿化解释了这一关系。随着通量的增加，3 keV以上的光谱也会软化，随着能量的增加而变得更强，直到200 keV。这表明电子温度和亮度之间存在反相关关系，可以用热吸积模型来解释。此外，我们还看到一个可变的宽带斜率，枢轴在200 keV。在软状态下，有一个高能量的尾巴与变化的幅度超出了强大的和可变的黑体组件。我们确认存在明显的滞后现象，硬到软的状态转换发生在更高的（和可变的）亮度比软到硬的过渡。我们拟合的RXTE/ASM数据与模型组成的外部吸积盘和热的内部流。然后，状态转换与圆盘截断半径的变化相关联，我们在软态下拟合为6 GM/c 2，在硬态下拟合为6 GM/c 2的几倍。内盘的消失发生在一个较低的吸积率比它的初始外观，由于源历史上的过渡的依赖性。我们提供了进一步的证据，反对在硬态的X射线辐射是非热同步辐射，并解释了所观察到的射电X射线相关的喷流功率与吸积功率。
We study X-ray and variability and distance of GX 339–4. We derive the distance of > 7 kpc, based on recent determination of the binary parameters. We study data from the ASM aboard Ginga, the BATSE aboard CGRO, and the ASM, PCA and HEXTE aboard RXTE. From 1987 to 2004, GX 339–4 underwent �15 outbursts and went through all known states of black-hole binaries. For the first time, we present the PCA data from the initial hard state of the outburst of 2004. We then study colourcolour and colour-flux correlations. In the hard state, there is a strong anticorrelation between the 1.5–5 and 3–12 keV spectral slopes, which we explain by thermal Comptonization of disc photons. There is also a softening of the spectrum above 3 keV with the increasing flux that becomes stronger with increasing energy up to �200 keV. This indicates an anticorrelation between the electron temperature and luminosity, explained by hot accretion models. In addition, we see a variable broad-band slope with a pivot at �200 keV. In the soft state, there is a high energy tail with varying amplitude beyond a strong and variable blackbody component. We confirm the presence of pronounced hysteresis, with the hard-to-soft state transitions occurring at much higher (and variable) luminosities than the soft-to-hard transitions. We fit the RXTE/ASM data with a model consisting of an outer accretion disc and a hot inner flow. State transitions are associated then with variations in the disc truncation radius, which we fit as � 6GM/c 2 in the soft state and several times that in the hard state. The disappearence of the inner disc takes place at a lower accretion rate than its initial appearance due to the dependence of the transitions on the source history. We provide further evidence against the X-ray emission in the hard state being nonthermal synchrotron, and explain the observed radio-X-ray correlation by the jet power being correlated with the accretion power.