论文标题
用于超轻深色黑暗黑暗探测的小行星检测
Asteroids for ultralight dark-photon dark-matter detection
论文作者
论文摘要
重力波（GW）探测器，该检测器监测惯性测试质量（TMS）之间分离的波动（TMS）对作用于这些TMS的新力敏感。超轻的深色暗物质（DPDM）耦合到$ u（1）_b $或$ u（1）_ {b-l} $充电提供一种力量，以DPDM质量设置的频率振荡。因此，在不同频带中运行的GW检测器对不同的DPDM质量范围敏感。基于监测内部太阳系中某些小行星的分离的最新GW检测建议将对$μ$ Hz频率具有敏感性[ARXIV：2112.11431]。在本文中，我们展示该建议还将如何启用DPDM的新参数空间的访问，并在质量范围内分别耦合到$ b $ [分别为$ b-l $]费用$ 5 \ [9] \ times 10^{ - 21} { - 21} \ text {ev} {ev} \ listsim m _ { \ text {ev} $，在$ m _ {\ m _ {\ text {$ \ varepsilon_b $ [$ \ varepsilon_b $ [$ \ varepsilon_ {b-l} $]上的最佳最佳限制的峰值敏感性超出了最佳限制。灵敏度最多可扩展到$ m _ {\ text {dm}} \ sim 2 \ times 10^{ - 18} \ text {ev} $仅当才能克服与小行星旋转运动相关的噪声问题时。
Gravitational-wave (GW) detectors that monitor fluctuations in the separation between inertial test masses (TMs) are sensitive to new forces acting on those TMs. Ultralight dark-photon dark matter (DPDM) coupled to $U(1)_B$ or $U(1)_{B-L}$ charges supplies one such force that oscillates with a frequency set by the DPDM mass. GW detectors operating in different frequency bands are thus sensitive to different DPDM mass ranges. A recent GW detection proposal based on monitoring the separation of certain asteroids in the inner Solar System would have sensitivity to $μ$Hz frequencies [arXiv:2112.11431]. In this paper, we show how that proposal would also enable access to new parameter space for DPDM coupled to $B$ [respectively, $B-L$] charges in the mass range $5\ [9] \times 10^{-21} \text{eV} \lesssim m_{\text{DM}} \lesssim 2 \times 10^{-19} \text{eV}$, with peak sensitivities about a factor of 500 [50] beyond current best limits on $\varepsilon_B$ [$\varepsilon_{B-L}$] at $m_{\text{DM}} \sim 2 \times 10^{-19} \text{eV}$. Sensitivity could be extended up to $m_{\text{DM}} \sim 2 \times 10^{-18} \text{eV}$ only if noise issues associated with asteroid rotational motion could be overcome.
