Magnetic support of the optical emission line filaments in NGC 1275
Magnetic support of the optical emission line filaments in NGC 1275
复制标题
DOI：
10.1038/nature07169
复制
发表时间：
2008-08
期刊：
影响因子：
64.8
通讯作者：
A. Fabian;R. Johnstone;J. Sanders;C. Conselice;C. S. Crawford;J. Gallagher;E. I. O. Astronomy;Cambridge;U. Nottingham;U. Wisconsin
中科院分区：
文献类型：
--
作者：
A. Fabian;R. Johnstone;J. Sanders;C. Conselice;C. S. Crawford;J. Gallagher;E. I. O. Astronomy;Cambridge;U. Nottingham;U. Wisconsin
巨大的椭圆星系NGC 1275位于英仙座星系团的中心，被一个著名的巨大的发射线丝状星云所包围，这些星云的年龄可能超过108岁。这些丝状体是被在炽热的团内气体中不断上升的无线电发射“气泡”从星系中心拖出来的，然后又回落。它们是能量从中心大质量黑洞转移到周围气体的反馈过程的标志。暗条是通过什么机制来抵抗潮汐切变并消散到周围极热（4 × 107K）的气体中的，目前还不清楚。在这里，我们报告的意见，解决丝状结构的细丝。有些线程超过6 kpc，但只有70 pc宽。我们的结论是，细丝中的磁场与周围的气体压力平衡，稳定了细丝，因此允许大量的冷气体积累并延迟星星的形成。
The giant elliptical galaxy NGC 1275, at the centre of the Perseus cluster, is surrounded by a well-known giant nebulosity of emission-line filaments,, which are plausibly in excess of 108years old. The filaments are dragged out from the centre of the galaxy by radio-emitting ‘bubbles’ rising buoyantly in the hot intracluster gas, before later falling back. They act as markers of the feedback process by which energy is transferred from the central massive black hole to the surrounding gas. The mechanism by which the filaments are stabilized against tidal shear and dissipation into the surrounding extremely hot (4 × 107K) gas has been unclear. Here we report observations that resolve thread-like structures in the filaments. Some threads extend over 6 kpc, yet are only 70 pc wide. We conclude that magnetic fields in the threads, in pressure balance with the surrounding gas, stabilize the filaments, so allowing a large mass of cold gas to accumulate and delay star formation.