Evolution and feedback of AGN jets of different cosmic ray composition
Evolution and feedback of AGN jets of different cosmic ray composition
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不同宇宙线成分的活动星系核喷流的演化与反馈
DOI：
10.1093/mnras/stad185
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发表时间：
2023
影响因子：
4.8
通讯作者：
Owen Ellis R
中科院分区：
文献类型：
--
作者：
Lin Yen-Hsing;Yang H-Y Karen;Owen Ellis R
来自活动星系核的喷流反馈是抑制冷核星系团冷却流的最有希望的机制之一。然而，活动星系核喷流和气泡的组成仍然不确定;它们可能是热主导的，或者是由宇宙射线质子（CRp）、宇宙射线电子（CRe）或磁能主导的。在这项工作中，我们调查的CRp和CRe占主导地位的喷流的演化和反馈效应进行三维磁流体动力学模拟AGN喷流膨胀气泡在团内介质中使用FLASH代码。我们提出了它们的能量，动力学和加热的演变，并模拟其预期的腔功率与射电光度的关系（Pcav-LR）。我们发现，气泡膨胀的CRe为主的射流遵循非常相似的动力学演化CRp为主的气泡，即使CRe内的气泡遭受显着更强的同步加速器和逆康普顿冷却。这是因为，当CRe失去能量时，喷射膨胀的气泡很快就在1.3亿年内成为热主导。它们的总能量随着CR能量的增加而停止下降，并且与CRp主导的气泡类似地演化。CRe和CRp占主导地位的气泡加热团内介质的能力也是相当的;通过局部热不稳定性形成的冷气在这两种情况下都得到了很好的抑制。CRp和CRe气泡在Pcav-LR平面上遵循不同的演化轨迹，但其值与FR-I源的观测范围大致一致。我们还讨论了观测技术，有可能约束AGN喷流和气泡的组成。
Jet feedback from active galactic nuclei (AGN) is one of the most promising mechanisms for suppressing cooling flows in cool-core clusters. However, the composition of AGN jets and bubbles remains uncertain; they could be thermally dominated, or dominated by cosmic ray proton (CRp), cosmic ray electron (CRe), or magnetic energy. In this work, we investigate the evolution and feedback effects of CRp and CRe dominated jets by conducting 3D magnetohydrodynamic simulations of AGN jet-inflated bubbles in the intracluster medium using the FLASH code. We present the evolution of their energies, dynamics, and heating, and model their expected cavity-power versus radio-luminosity relation (Pcav–LR). We find that bubbles inflated by CRe dominated jets follow a very similar dynamical evolution to CRp dominated bubbles even though CRe within bubbles suffer significantly stronger synchrotron and inverse-Compton cooling. This is because, as CRe lose their energy, the jet-inflated bubbles quickly become thermally dominated within ∼30 Myr. Their total energy stops decreasing with CR energy and evolves similarly to CRp dominated bubbles. The ability of CRe and CRp dominated bubbles to heat the intracluster medium is also comparable; the cold gas formed via local thermal instabilities is well suppressed in both cases. The CRp and CRe bubbles follow different evolutionary trajectories on thePcav–LRplane, but the values are broadly consistent with observed ranges for FR-I sources. We also discuss observational techniques that have potential for constraining the composition of AGN jets and bubbles.