未来引力波观测站试验物质的气体冷却
Gas cooling of test masses for future gravitational-wave observatories
摘要：
先进LIGO和先进Virgo的最新观测开启了引力波天文学的时代。这些“第二代”（2G）地面观测站检测到的事件数量部分受到用于探测时空动力学的测试质量镜表面温度引起的位置波动所产生的噪声的限制。下一代引力波观测站的设计通过使用低温冷却的测试质量来解决这一限制;目前用于连续去除热量（由吸收的激光产生）的方法依赖于通过黑体辐射或通过悬浮纤维传导的热量提取。作为一种补充方法，在观测运行过程中提取热量，我们研究冷却通过氦气冲击在自由分子流中的测试质量。我们建立了冷却功率和相应的位移噪声之间的关系，基于分析模型，我们比较数值模拟。应用这个理论框架的概念设计的爱因斯坦望远镜（ET），我们发现一个冷却功率为10毫瓦，在18 K的气体压力超过ET设计应变噪声目标的最多一个因素的$\sim 3$在信号频带从3到11赫兹。在18 K下100 mW的冷却功率对应于在从1到28 Hz的频带中超过ET设计应变噪声目标最多$\sim 11$倍的气体压力。
英文摘要：
Recent observations made with Advanced LIGO and Advanced Virgo have initiated the era of gravitational-wave astronomy. The number of events detected by these "2nd Generation" (2G) ground-based observatories is partially limited by noise arising from temperature-induced position fluctuations of the test mass mirror surfaces used for probing spacetime dynamics. The design of next-generation gravitational-wave observatories addresses this limitation by using cryogenically cooled test masses; current approaches for continuously removing heat (resulting from absorbed laser light) rely on heat extraction via black-body radiation or conduction through suspension fibres. As a complementing approach for extracting heat during observational runs, we investigate cooling via helium gas impinging on the test mass in free molecular flow. We establish a relation between cooling power and corresponding displacement noise, based on analytical models, which we compare to numerical simulations. Applying this theoretical framework with regard to the conceptual design of the Einstein Telescope (ET), we find a cooling power of 10 mW at 18 K for a gas pressure that exceeds the ET design strain noise goal by at most a factor of $\sim 3$ in the signal frequency band from 3 to 11 Hz. A cooling power of 100 mW at 18 K corresponds to a gas pressure that exceeds the ET design strain noise goal by at most a factor of $\sim 11$ in the band from 1 to 28 Hz.
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