Searching for dark clumps with gravitational-wave detectors
Searching for dark clumps with gravitational-wave detectors
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DOI：
10.1103/physrevd.106.063015
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发表时间：
2022-06
影响因子：
5
通讯作者：
S. Baum;M. Fedderke;P. Graham
中科院分区：
文献类型：
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作者：
S. Baum;M. Fedderke;P. Graham
经过太阳系的黑暗致密物体（“团块”）对引力波（GW）探测器中的测试质量（TM）施加加速度。我们在各种当前和未来的GW探测器中重新检查这些团簇跃迁的可探测性，在广泛的频率范围内工作。由团块穿越内太阳系引起的TM加速度的频率含量在f ~µHz左右。我们中的一些人[Fedderke等人]。、phy。Rev. D 105, 103018(2022)]最近提出了一种基于小行星到小行星测距的毫瓦探测概念，灵敏度为µHz。从这一概念的详细灵敏度投影中，我们在分析和模拟中都发现，如果质量为cm ~ 10 ~ 14 kg的团块使暗物质（DM）密度饱和，则纯引力团块-物质相互作用将每~ 20年产生一次可探测的过境。其他（提议的）使用本地TMs的GW探测器，在更高的频段工作，对较小的团块质量敏感，并且具有较小的可发现信号率。我们还考虑了团块被赋予额外的具有吸引力的远距离团块物质第五种力的情况，这种力比引力强得多（但逃避了已知的第五种力的约束）。为µ赫兹探测器的概念,我们使用模拟表明,例如,一个clump-matter第五力量∼10 3倍重力与一系列∼盟会提高检测的速度凌日每年几块的质量范围10 11公斤(cid: 46) m cl (cid: 46) 10 14公斤,即使它们∼1% DM的子组件。µ赫兹GW探测器来探测的能力asteroid-mass-scale黑暗的对象,否则可能无法觉察的支持了科学的发展。
Dark compact objects (“clumps”) transiting the Solar System exert accelerations on the test masses (TM) in a gravitational-wave (GW) detector. We reexamine the detectability of these clump transits in a variety of current and future GW detectors, operating over a broad range of frequencies. TM accelerations induced by clump transits through the inner Solar System have frequency content around f ∼ µ Hz. Some of us [Fedderke et al ., Phys. Rev. D 105 , 103018 (2022)] recently proposed a GW detection concept with µ Hz sensitivity, based on asteroid-to-asteroid ranging. From the detailed sensitivity projection for this concept, we find both analytically and in simulation that purely gravitational clump–matter interactions would yield one detectable transit every ∼ 20 yrs, if clumps with mass m cl ∼ 10 14 kg saturate the dark-matter (DM) density. Other (proposed) GW detectors using local TMs and operating in higher frequency bands are sensitive to smaller clump masses and have smaller rates of discoverable signals. We also consider the case of clumps endowed with an additional attractive long-range clump–matter fifth force significantly stronger than gravity (but evading known fifth-force constraints). For the µ Hz detector concept, we use simulations to show that, for example, a clump–matter fifth-force ∼ 10 3 times stronger than gravity with a range of ∼ AU would boost the rate of detectable transits to a few per year for clumps in the mass range 10 11 kg (cid:46) m cl (cid:46) 10 14 kg, even if they are a ∼ 1 % sub-component of the DM. The ability of µ Hz GW detectors to probe asteroid-mass-scale dark objects that may otherwise be undetectable bolsters the science case for their development.