arXiv 0810.15192008-10-08astro-ph

天鹅座X-1的朱雀观测

Suzaku Observations of Cyg X-1

Michael A. Nowak

备注：: 10 pages. Contributed talk at the 7th Microquasar Workshop, Foca, Turkey, Sept. 1-5, 2008
发表信息：: PoS MQW7:030,2008

摘要：

我们目前的亮点，从一系列的四个同时朱雀/RXTE观测的黑洞候选人天鹅座X-1。我们简要总结了我们长达十年的RXTE监测活动的几个关键结果。然后，我们评论分析朱雀数据的挑战，即，改进现有工具之外的方位校正，并定量评估堆积。我们所有的朱雀观测（一个，根据设计）都发生在或非常接近轨道相位0（优合），因此显示了颜色-颜色图的演变，这是由于次级风中的物质吸收X射线所致。我们提出了简单的部分吸收模型，这种演变。然后，我们比较朱雀和RXTE数据，并明确划分为窄和宽的组成部分的Fe线区域。两者都是朱雀数据所必需的，并且被认为与RXTE数据一致。这些朱雀观测发生在历史上硬，低通量状态附近。我们提出了一个简单的唯象破幂律模型，以及一个更具物理动机的康普顿化模型的宽带光谱。虽然前一类模型比任何物理模型都更好地描述了几乎所有的RXTE活动，但后一类模型稍微更成功。康普顿化模型，然而，表现出一个软磁盘组件，这在形式上对应于一个小的，内盘半径的证据很少。这是否是物理的，由于未建模的吸收，或者是一个校准问题，仍然是一个悬而未决的问题。

英文摘要：

We present highlights from a series of four simultaneous Suzaku/RXTE observations of the black hole candidate Cyg X-1. We briefly summarize several key results from our decade long RXTE monitoring campaign. We then comment on challenges of analyzing the Suzaku data, i.e., improving the aspect correction beyond that of the existing tools, and quantitatively assessing pileup. All of our Suzaku observations (one, by design) occurred at or very near orbital phase 0 (superior conjunction), and hence show evolution in color-color diagrams due to X-ray absorption by material from the wind of the secondary. We present simple partial absorption models for this evolution. We then compare the Suzaku and RXTE data, and explicitly divide the Fe line region into narrow and broad components. Both are required for the Suzaku data, and are seen to be consistent with the RXTE data. These Suzaku observations occurred near historically hard, low flux states. We present fits of the broad band spectra with a simple phenomenological broken powerlaw model, as well as a more physically motivated Comptonization model. Whereas the former class of models described nearly all of the RXTE campaign better than any physical model, here the latter model is slightly more successful. The Comptonization model, however, exhibits little evidence for a soft disk component, which formally corresponds to a small, inner disk radius. Whether this is physical, due to unmodeled absorption, or is a calibration issue, remains an open question.

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