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首页> 外文期刊>The Astrophysical journal >ON THE ORIGIN OF TEMPERATURE SUBSTRUCTURE WITHIN MERGING CLUSTERS OF GALAXIES: ABELL 2256
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ON THE ORIGIN OF TEMPERATURE SUBSTRUCTURE WITHIN MERGING CLUSTERS OF GALAXIES: ABELL 2256

机译：关于合并星系群中的温度子结构的起源：ABELL 2256

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摘要

Recent ROSAT PSPC and ASCA observations of several rich clusters of galaxies have revealed complex temperature substructure within the X-ray emitting gas. One of the best and most detailed examples is A2256. Briel & Henry (1994) show four distinct temperature components within the central (< 12′) of A2256. The purpose of this paper is to suggest a plausible model, within reasonable parameter space, that explains the origin of the hottest (> 8 keV) gas near the core of A2256. We find the temperature substructure in A2256 to be consistent with a model in which A2256 is currently in the early stages of a merger. We attempt to quantify this model by comparison with results from our parameter study of merging clusters of galaxies conducted with a numerical Hydro/N-body code. From this, we estimate that A2256 is actually two systems with a 2:1 mass ratio, whose cores are separated by ～0.5 Mpc with a relative velocity of nearly 3000 km s~(-1). The proposed merger axis is projected into the plane of the sky by 45°-50° such that the less massive of the two clusters is approaching the observer. Within the frame work of this model, we find the hot gas (> 8 keV) to be the result of shock heating during the merger event. We also use this model to explain the discrepancy between X-ray and galaxy-based mass estimates for A2256.
机译：最近的ROSAT PSPC和ASCA对几个星系的富星团的观测揭示了X射线发射气体中复杂的温度子结构。最好和最详细的例子之一是A2256。 Briel＆Henry（1994）显示了A2256中心（<12'）内的四个不同的温度分量。本文的目的是在合理的参数空间内提出一个合理的模型，该模型解释A2256核心附近最热（> 8 keV）气体的起源。我们发现A2256中的温度子结构与A2256当前处于合并初期的模型是一致的。我们试图通过与使用数值Hydro / N体代码进行的合并星系团的参数研究的结果进行比较，来量化该模型。据此，我们估计A2256实际上是两个质量比为2：1的系统，其核心之间的间隔为〜0.5 Mpc，相对速度接近3000 km s〜（-1）。拟议的合并轴以45°-50°的角度投影到天空平面中，从而使两个星团中质量较小的那个接近观察者。在此模型的框架内，我们发现热气（> 8 keV）是合并事件期间震动加热的结果。我们还使用此模型来解释X射线和基于A2256的基于星系的质量估计之间的差异。

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