绝热压缩的波暗物质晕与中等质量比旋近
Adiabatically compressed wave dark matter halo and intermediate-mass ratio inspirals
AI总结：
本文研究波暗物质晕在中心黑洞绝热增长下的压缩效应，发现压缩后密度显著增强并影响中等质量比旋近的引力波相位，为未来引力波探测重建波暗物质晕提供依据。
摘要：
中心大质量黑洞的绝热增长会压缩其周围的暗物质晕，导致暗物质晕的密度轮廓变得更陡，这一现象被称为绝热压缩。我们研究波暗物质的绝热压缩——波暗物质是一种质量小于几电子伏特的轻玻色子暗物质候选体。利用绝热定理，我们证明绝热压缩会导致一个密度远高于粒子暗物质晕的波暗物质晕，在半经典极限下与粒子暗物质晕相似。压缩后的波暗物质晕在中心区域与粒子暗物质晕不同，因为半经典近似在该区域失效；中心轮廓取决于暗物质质量与中心黑洞质量，它们共同决定孤子态和低角动量模式能否在天体物理时间尺度上存活而不被黑洞吸收。这种压缩轮廓具有若干天体物理意义。作为一个例子，我们研究了波暗物质晕中中心中等质量黑洞与致密太阳质量天体之间旋近产生的引力波。由于质量密度增强，压缩后的波暗物质晕对绕转天体施加更强的动力学摩擦，导致引力波相位偏移。这种相位偏移模式与粒子暗物质晕中的旋近不同，原因在于密度轮廓的差异以及源自暗物质波动性质的相对受抑制的动力学摩擦力。我们研究了未来引力波探测器（如激光干涉仪空间天线）的前景，并确定了可以通过引力波观测重建波暗物质晕的物理场景。
英文摘要：
The adiabatic growth of a central massive black hole could compress the surrounding dark matter halo, leading to a steeper profile of the dark matter halo. This phenomenon is called adiabatic compression. We investigate the adiabatic compression of wave dark matter - a light bosonic dark matter candidate with its mass smaller than a few eV. Using the adiabatic theorem, we show that the adiabatic compression leads to a much denser wave dark matter halo similar to the particle dark matter halo in the semiclassical limit. The compressed wave halo differs from that of the particle halo near the center where the semiclassical approximation breaks down, and the central profile depends on dark matter and the central black hole mass as they determine whether the soliton and low angular momentum modes can survive over the astrophysical time scale without being absorbed by the black hole. Such a compressed profile has several astrophysical implications. As one example, we study the gravitational waves from the inspiral between a central intermediate-mass black hole and a compact solar-mass object within the wave dark matter halo. Due to the enhanced mass density, the compressed wave dark matter halo exerts stronger dynamical friction on the orbiting object, leading to the dephasing of the gravitational waves. The pattern of dephasing is distinctive from that of inspirals in the particle dark matter halo because of the difference in density profile and because of the relatively suppressed dynamical friction force, originating from the wave nature of dark matter. We investigate the prospects of future gravitational wave detectors, such as Laser Interferometer Space Antenna, and identify physics scenarios where the wave dark matter halo can be reconstructed from gravitational wave observations.
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