标题： 宇宙射线的爱丁顿极限：低质量射电明亮类星体观测缺失以及 M_{BH}-M_{隆起}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 Low-Mass 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星系核球在无线电活跃类星体活动时期的操作。 在相对论性类星体喷流的射电核中，内部冲击波将一部分有序的动能转化为随机化的相对论性离子，换句话说就是宇宙射线。 通过采用基于现象学的喷流模型，我们表明足够多的能量在1-100 GeV范围内的宇宙射线从射电核逃逸到宿主星系中，从而突破了宇宙射线的爱丁顿极限。 因此，流体静力平衡被破坏，并发展出一种由宇宙射线动量驱动的风，将气体从宿主星系中排出，从而自我限制了黑洞和核球的增长。 尽管星际空间的宇宙射线功率远小于类星体光子的亮度，但由于宇宙射线与星系气体交换动量的效率更高，它们提供的反馈比紫外线光子更强。 每单位黑洞静止质量能量释放到宿主星系中的宇宙射线能量与黑洞质量无关。 由此可知，射电明亮的喷流应该在相对较重的系统中更为普遍，因为它们位于具有相对深引力势的星系中。 因此，由喷流驱动的宇宙射线反馈不仅自我调节了黑洞和核球的增长，还解释了相对较小星系中缺乏射电明亮活动的原因。 通过使用有关射电核物理条件的基本已知事实，我们近似地再现了M_{BH}-M_{隆起}关系的斜率和归一化值。 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 1-100 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.