轴对称对数势描述的卫星星系上由模糊暗物质产生的动力学摩擦
Dynamical Friction due to fuzzy dark matter on satellites described by axisymmetric logarithmic potentials
AI总结：
本研究针对超轻玻色子构成的模糊暗物质，模拟了非球对称卫星星系穿过其晕时的动力学摩擦，发现尾迹特征、阻力大小受卫星形状和运动方向影响显著，且相关时标接近哈勃时间。
摘要：
一种合理的暗物质候选体是被称为模糊暗物质（fuzzy dark matter，简称FDM）的超轻玻色子。模糊暗物质玻色子的等效质能约为$10^{-22}$eV，对应的德布罗意波长达到千秒差距量级，因此在与星系核心相当的尺度上表现出波动行为，这是传统冷暗物质模型中不会出现的特性。星系团中模糊暗物质的存在会通过动力学摩擦影响其成员的运动。在本研究中，我们对穿过初始均匀模糊暗物质晕的卫星星系所受的动力学摩擦开展了模拟研究。我们重点关注形状超出球对称的卫星星系，这类星系由椭球势和对数势描述。我们发现，此类卫星星系穿行时在模糊暗物质晕中产生的尾迹，与球对称卫星星系产生的尾迹存在定性差异。此外，我们量化了这类系统的动力学摩擦系数，发现同一卫星星系所受的阻力可能因自身椭率和运动方向的不同而相差5倍。最后，我们假设一个质量为$10^{11}$M$_{\text{⊙}}$的卫星星系以$10^3$km/s的速度穿过平均密度约为$10^6$M$_{\bot}$kpc$^{-3}$的FDM晕，计算得到其动力学摩擦时标接近哈勃时间。
英文摘要：
A plausible dark matter candidate is an ultralight bosonic particle referred to as fuzzy dark matter. The equivalent mass-energy of the fuzzy dark matter boson is $\sim 10^{-22}$eV and has a corresponding de Broglie wavelength of kiloparsec scale, thus exhibiting wave behaviour in scales comparable to a galactic core, which could not appear in conventional cold dark matter models. The presence of fuzzy dark matter in galactic clusters will impact the motion of their members through dynamical friction. In this work, we present simulations of the dynamical friction on satellites traversing an initially uniform fuzzy dark matter halo. We focus on the satellites whose shapes are beyond spherical symmetry described by ellipsoidal and logarithmic potentials. We find that the wakes created on the fuzzy dark matter halo due to the passage of such satellites are qualitatively different from those generated by spherically symmetric ones. Furthermore, we quantify the dynamical friction coefficient for such systems, finding that the same satellite may experience a drag differing by a factor of $5$ depending on its ellipticity and the direction of motion. Finally, we find that the dynamical friction time-scale is close to Hubble time, assuming a satellite of $10^{11}$M$_{\odot}$ traversing at $10^{3}$km/s a FDM halo whose mean density is $\sim 10^6$M$_{\odot}$kpc$^{-3}$.
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