The response of ultralight dark matter to supermassive black holes and binaries
The response of ultralight dark matter to supermassive black holes and binaries
复制标题
超轻暗物质对超大质量黑洞和双星的响应
DOI：
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发表时间：
2020
期刊：
影响因子：
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通讯作者：
R. Vicente
中科院分区：
文献类型：
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作者：
L. Annulli;V. Cardoso;R. Vicente
标量场可以产生受限结构，如玻色子星或q球。这些物体是有趣的假想的新“暗物质恒星”，但也很好地描述了当磁场超轻时的暗物质晕。在这里，我们研究了这种受限玻色子结构在其附近被外部物质（恒星、行星或黑洞）激发时的动力学响应。这样的扰动可以穿过玻色子构型，也可以简单地作为周期源。我们的设置还可以有效地描述大质量黑洞与周围环境之间的相互作用，在大质量物体经历了“踢”之后不久，由于银河系中心重子物质的崩溃。它还将暗物质消耗描述为对光晕内激发双星的反应。我们计算了在这些过程中辐射的总能量损失、线动量和角动量，并在这些背景下执行了作用于运动物体的动力摩擦的第一次自一致计算。我们证明了牛顿玻色子恒星（NBS）中心的超大质量黑洞的引力坍缩伴随着周围核心的微小变化。NBS最终会被吸积，但从天体物理参数的角度来看，其吸积幅度仅为哈勃尺度的1倍。恒星或超大质量双星能够“搅拌”并从NBS中排出标量。对于LIGO或LISA波段中接近聚并的双星，标量发射影响了相对于主导四极项的前$-6$ PN阶的波形；该系数太小，无法被下一代干涉仪探测到。我们的研究结果提供了黑洞或恒星与它们所处的超轻暗物质环境之间相互作用的完整图景。
Scalar fields can give rise to confined structures, such as boson stars or Q-balls. These objects are interesting hypothetical new"dark matter stars,"but also good descriptions of dark matter haloes when the fields are ultralight. Here, we study the dynamical response of such confined bosonic structures when excited by external matter (stars, planets or black holes) in their vicinities. Such perturbers can either be plunging through the bosonic configuration or simply act as periodic sources. Our setup can also efficiently describe the interaction between a massive black hole and the surrounding environment, shortly after the massive body has undergone a"kick", due to the collapse of baryonic matter at the galactic center. It also depicts dark matter depletion as a reaction to an inspiralling binary within the halo. We calculate total energy loss, and linear and angular momenta radiated during these processes, and perform the first self-consistent calculation of dynamical friction acting on moving bodies in these backgrounds. We show that the gravitational collapse to a supermassive black hole at the center of a Newtonian boson star (NBS) is accompanied by a small change in the surrounding core. The NBS eventually gets accreted, but only on times larger than a Hubble scale for astrophysical parameters. Stellar or supermassive binaries are able to"stir"and expel scalar from the NBS. For binaries in the LIGO or LISA band, close to coalescence, scalar emission affects the waveform at leading $-6$ PN order with respect to the dominant quadrupolar term; the coefficient is too small to allow detection by next-generation interferometers. Our results provide a complete picture of the interaction between black holes or stars and the ultralight dark matter environment they live in.