Plasmas of geometrically thick, black hole (BH) accretion flows in active galactic nuclei (AGNs) are generally collisionless for protons, and involve magnetic field turbulence. Under such conditions a fraction of protons can be accelerated stochastically and create relativistic neutrons via nuclear collisions. These neutrons can freely escape from the accretion flow and decay into protons in the dilute polar region above the rotating BH to form relativistic jets. We calculate geometric efficiencies of the neutron energy and mass injections into the polar region, and show that this process can deposit luminosity as high as and mass loading for the case of the BH mass M ~ 108 M ☉, where is the mass accretion rate. The terminal Lorentz factors of the jets are Γ ~ 3, and they may explain the AGN jets having low luminosities. For higher luminosity jets, which can be produced by additional energy inputs such as Poynting flux, the neutron decay still can be a dominant mass loading process, leading to, e.g., Γ ~ 50 for .
展开▼
机译：活跃的银河原子核（AGN）中具有几何形状厚实的黑洞（BH）积聚的等离子体对于质子通常是无碰撞的，并且涉及磁场湍流。在这种情况下，一部分质子可以随机加速，并通过核碰撞产生相对论中子。这些中子可以自由地从积聚流中逸出，并在旋转的BH上方的稀极性区域中衰减成质子，从而形成相对论射流。我们计算了中子能量和注入极区的质量的几何效率，并表明对于BH质量为M〜108 M case的情况，该过程可以沉积高达和高负荷的光度，其中BH为质量积聚率。射流的终端洛伦兹因子为Γ〜3，它们可以解释AGN射流的光度低。对于可以通过附加能量输入（例如Poynting通量）产生的更高光度的射流，中子衰变仍然可能是主要的质量加载过程，例如导致Γ〜50。
展开▼
