论文标题
活性银河核中潮汐破坏事件的光曲线
Light curves of tidal disruption events in active galactic nuclei
论文作者
论文摘要
活性银河核的黑洞被吸积盘包围。磁盘的表面密度总是太低而无法影响恒星的潮汐破坏，但是它可能足够高，以至于当碎屑流返回到周围并通过磁盘打孔时会产生剧烈的相互作用。磁盘上激发的冲击会消散磁盘内部的动能到影响点，并加快向黑洞的流入。具有光度$ \ gtrsim10^{ - 3} $的辐射有效磁盘具有足够高的表面密度，以至于初始的流盘相互作用以超级 - 埃德丁顿的速率导致能量消散。由于流入迅速，只有部分消散的能量作为辐射出现，而其余的则将其推入黑洞。耗散，流入和冷却平衡，以保持降压仪的辐射光度，其持续时间为数十天，几乎是线性依赖于恒星质量的。高原之后，亮度与磁盘表面密度成比例降低，较早时期的幂律指数在$ -3 $和$ -2 $之间，并且可能在以后的陡峭指数。
The black hole of an active galactic nucleus is encircled by an accretion disk. The surface density of the disk is always too low to affect the tidal disruption of a star, but it can be high enough that a vigorous interaction results when the debris stream returns to pericenter and punches through the disk. Shocks excited in the disk dissipate the kinetic energy of the disk interior to the impact point and expedite inflow toward the black hole. Radiatively efficient disks with luminosity $\gtrsim10^{-3}$ Eddington have a high enough surface density that the initial stream-disk interaction leads to energy dissipation at a super-Eddington rate. Because of the rapid inflow, only part of this dissipated energy emerges as radiation, while the rest is advected into the black hole. Dissipation, inflow, and cooling balance to keep the bolometric luminosity at an Eddington-level plateau whose duration is tens of days, with an almost linear dependence on stellar mass. After the plateau, the luminosity decreases in proportion to the disk surface density, with a power-law index between $-3$ and $-2$ at earlier times, and possibly a steeper index at later times.
