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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Suzaku observations of spectral variations of the ultra-luminous X-ray source Holmberg IX X-1
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Suzaku observations of spectral variations of the ultra-luminous X-ray source Holmberg IX X-1

机译：Suzaku观察超光X射线源Holmberg IX X-1的光谱变化

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摘要

Observations of the ultra-luminous X-ray source (ULX) Holmberg IX X-1 were carried out with Suzaku twice, once on 2012 April 13 and then on 2012 October 24, with exposures of 180 ks and 217 ks, respectively. The source showed a hard power-law shaped spectrum with a mild cutoff at similar to 8 keV, which is typical of ULXs when they are relatively dim. On both occasions, the 0.6-11 keV spectrum was explained successfully in terms of a cool (similar to 0.2 keV) multi-color disk blackbody emission model and thermal Comptonization emission produced by an electron cloud with a relatively low temperature and high optical depth, assuming that a large fraction of the disk-blackbody photons are Comptonized whereas the rest are observed directly. The 0.5-10 keV luminosity was 1.2 x 10(40) erg s(-1) in April, and similar to 14% higher in October. This brightening was accompanied by spectral softening in >= 2 keV, with little change in the <= 2 keV spectral shape. This behavior can be understood if the accretion disk remains unchanged while the electron cloud covers a variable fraction of the disk. The absorbing column density was consistent with the galactic line-of sight value, and did not vary by more than 1.6 x 10(21) cm(-2). Together with the featureless spectra, these properties may not be reconciled easily with the supercritical accretion scenario of this source.
机译：使用Suzaku对超发光X射线源（ULX）Holmberg IX X-1进行了两次观测，一次是在2012年4月13日，然后是在2012年10月24日，曝光量分别为180 ks和217 ks。源显示出一个硬幂律形状的光谱，在类似于8keV的情况下有一个温和的截止，这是ULX在相对较暗时的典型情况。在这两种情况下，0.6-11千电子伏的光谱都成功地用一个冷却（类似于0.2千电子伏）的多色圆盘黑体发射模型和一个温度相对较低、光学深度较高的电子云产生的热Comptonization发射来解释，假设大部分圆盘黑体光子是Comptonization的，而其余的光子是直接观察到的。4月份的0.5-10千电子伏光度为1.2 x 10（40）erg s（-1），与10月份的14%相似。这种增亮伴随着大于等于2千电子伏的光谱软化，而小于等于2千电子伏的光谱形状几乎没有变化。如果吸积盘保持不变，而电子云覆盖着吸积盘的可变部分，则可以理解这种行为。吸收柱密度与银河系视线值一致，变化不超过1.6 x 10（21）cm（-2）。加上无特征的光谱，这些性质可能不容易与该源的超临界吸积情景相协调。

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