标题： 宇宙射线中的爱丁顿极限：对观测到的无无线电波类星体和 M_{BH}-M_{凸起}关系的解释 显示英文标题

标题： The Eddington Limit in Cosmic Rays: An Explanation for the Observed Lack of Radio-Loud Quasars and the M_{BH}-M_{Bulge} Relation

摘要： 我们提出了一种反馈机制，用于超大质量黑洞及其宿主核球，在射电安静类星体活动时期起作用。 在相对论性类星体喷流的射电核心中，内部激波将一部分有序的整体动能转化为随机化的相对论离子，换句话说就是宇宙射线。 通过采用一种现象学驱动的喷流模型，我们表明足够多的1-10 GeV宇宙射线可以从射电核心逃逸到宿主星系，从而在宇宙射线上打破爱丁顿极限。 结果是，流体静力平衡被破坏，并发展出由宇宙射线动量驱动的风，将气体从宿主星系中排出，从而自我限制黑洞和核球的增长。 尽管星际宇宙射线功率远小于类星体光度，但宇宙射线提供的反馈比紫外光子更强，因为它们与星系气体交换动量的效率更高。 以单位黑洞静止质量能量释放到宿主星系中的能量，与黑洞质量无关。 因此，射电明亮喷流应该在相对较高质量的系统中更为普遍，因为它们位于具有相对较深引力势的星系中。 因此，由喷流驱动的宇宙射线反馈不仅自我调节黑洞和核球的增长，还提供了一个解释，即为什么相对较小的星系缺乏射电明亮活动。 通过利用关于射电核心物理条件的基本已知事实，我们近似地重现了M_{BH}-M_{凸起}关系的斜率和归一化。 显示英文摘要

摘要： We present a feedback mechanism for supermassive black holes and their host bulges that operates during epochs of radio-loud quasar activity. In the radio cores of relativistic quasar jets, internal shocks convert a fraction of ordered bulk kinetic energy into randomized relativistic ions, or in other words cosmic rays. By employing a phenomenologically-motivated jet model, we show that enough 1-10 GeV cosmic rays escape the radio core into the host galaxy to break the Eddington limit in cosmic rays. As a result, hydrostatic balance is lost and a cosmic ray momentum-driven wind develops, expelling gas from the host galaxy and thus self-limiting the black hole and bulge growth. Although the interstellar cosmic ray power is much smaller than the quasar photon luminosity, cosmic rays provide a stronger feedback than UV photons, since they exchange momentum with the galactic gas much more efficiently. The amount of energy released into the host galaxy as cosmic rays, per unit of black hole rest mass energy, is independent of black hole mass. It follows that radio-loud jets should be more prevalent in relatively massive systems since they sit in galaxies with relatively deep gravitational potentials. Therefore, jet-powered cosmic ray feedback not only self-regulates the black hole and bulge growth, but also provides an explanation for the lack of radio-loud activity in relatively small galaxies. By employing basic known facts regarding the physical conditions in radio cores, we approximately reproduce both the slope and the normalization of the M_{BH}-M_{Bulge} relation.