用大质量慢喷流解释MS0735 +7421的高能AGN爆发
Explaining the Energetic AGN Outburst of MS0735+7421 with Massive Slow Jets
摘要：
通过进行轴对称流体动力学数值模拟（2.5维代码），我们表明，缓慢，大规模，宽射流可以重现星系团MS 0735 +7421中的巨大的X射线缺陷气泡对的形态。由气泡对和冲击波中的能量组成的射流的总能量被McNamara等人（2009）进行的观测限制为~10^{62}erg。我们发现，两个相对的喷流是活跃的~ 100 Myr，每个发射半开角~70度，初始速度~0.1c，和两个喷流的总质量损失率~100 Mo/年，可以解释所观察到的形态。可以使用快速旋进的窄射流来代替宽射流。在我们的模型中，星团在大约1亿年前遭受了一次冷却灾难。大部分被冷却的质量，~10^{10} Mo，被AGN活动驱逐回团内介质（ICM），现在在气泡内，~10%形成恒星，~10%的冷气体被中心黑洞吸积，是爆发能量的来源。这种类型的活动类似于预期在星系形成中发生的活动。
英文摘要：
By conducting axisymmetrical hydrodynamical numerical simulations (2.5 dimensional code) we show that slow, massive, wide jets can reproduce the morphology of the huge X-ray deficient bubble pair in the cluster of galaxies MS0735+7421. The total energy of the jets, composed of the energy in the bubble pair and in the shock wave, is constraint by observations conducted by McNamara et al. (2009) to be ~10^{62}erg. We show that two opposite jets that are active for ~100Myr, each with a launching half opening angle of ~70 degrees, an initial velocity of ~0.1c, and a total mass loss rate of the two jets of ~100 Mo/year, can account for the observed morphology. Rapidly precessing narrow jets can be used instead of wide jets. In our model the cluster suffered from a cooling catastrophe ~100Myr ago. Most of the mass that cooled, ~10^{10} Mo, was expelled back to the intracluster medium (ICM) by the AGN activity and is inside the bubbles now, ~10% formed stars, and ~10% of the cold gas was accreted by the central black hole and was the source of the outburst energy. This type of activity is similar to that expected to occur in galaxy formation.
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