暗物质（DM）直接探测实验在DM质量大于几GeV时对DM-核子散射截面有很强的限制，但在低质量区留下了很大的参数空间。如果DM能在直接探测实验中产生核反冲以提供可观测的信号，那么它很可能会被膨胀宇宙中的相对论性宇宙射线散射和增强。由于使用锗的低能量阈值探测器对普通晕GeV尺度DM提供了良好的约束，因此有必要重新分析CDEX-10实验中102.8 kg $\times$天的数据，假设DM由宇宙射线增强。对于DM质量范围为1 keV的$<m_χ<$ ~ 1 MeV，有效距离在1 kpc以内的情况，在90%的置信水平下，我们在$8.32\times10^{-30}$ cm $^2$处得到了自旋无关的DM-核子散射截面上几乎平坦的下限. CDEX-10的结果是能够关闭的MiniBooNE和XENON 1 T约束之间的参数空间，这是部分地阻碍了地球衰减效应之间的差距明确。我们还定量计算了预期的中微子地板上寻找CRBDM在未来的直接检测实验使用锗。
英文摘要：
Dark matter (DM) direct detection experiments have been setting strong limits on the DM-nucleon scattering cross section at the DM mass above a few GeV, but leave large parameter space unexplored in the low mass region. DM is likely to be scattered and boosted by relativistic cosmic rays in the expanding universe if it can generate nuclear recoils in direct detection experiments to offer observable signals. Since low energy threshold detectors using Germanium have provided good constraints on ordinary halo GeV-scale DM, it is necessary to re-analyze 102.8 kg$\times$day data in the CDEX-10 experiment assuming that DM is boosted by cosmic rays. For the DM mass range 1 keV $<m_χ<$ 1 MeV and the effective distance within 1 kpc, we reach an almost flat floor limit at $8.32\times10^{-30}$ cm$^2$ on spin-independent DM-nucleon scattering cross section at a 90\% confidence level. The CDEX-10 result is able to close the gap unambiguously in the parameter space between MiniBooNE and XENON1T constraints which was partially hindered by the Earth attenuation effect. We also quantitatively calculate expected neutrino floor on searching for CRBDM in future direct detection experiments using Germanium.
Constraints on dark matter boosted by supernova shock within the effective field theory framework from the CDEX-10 experiment
Tsinghua University（清华大学）；Academia Sinica（中央研究院）；Beijing Normal University（北京师范大学）；Sichuan University（四川大学）；Peking University（北京大学）；China Institute of Atomic Energy（中国原子能科学研究院）；Sun Yat-sen University（中山大学）；Nankai University（南开大学）；Banaras Hindu University（贝拿勒斯印度教大学）
Dark Parton Shower Effects for Cosmic Ray Boosted Dark Matter
College of Physics, Sichuan University（四川大学物理学院）；Institute of Physics, Henan Academy of Sciences（河南省科学院物理研究所）；Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所）
Cosmic-ray boosted inelastic dark matter from neutrino-emitting active galactic nuclei
Virginia Tech（弗吉尼亚理工大学）；Massachusetts Institute of Technology（麻省理工学院）；Harvard University（哈佛大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；Fermi National Accelerator Laboratory（费米国家加速实验室）；University of Chicago（芝加哥大学）
Cosmic Ray Boosted Dark Matter in COSINUS: Modeling and Constraints
Max-Planck-Institut für Physik（马克斯·普朗克物理研究所）；Marietta-Blau-Institut für Teilchenphysik der Österreichischen Akademie der Wissenschaften（奥地利科学院玛丽塔·布劳粒子物理研究所）；Atominstitut, Technische Universität Wien（维也纳工业大学原子研究所）；INFN - Sezione di Roma（罗马国家核物理研究所分部）；Gran Sasso Science Institute（格兰萨索科学研究所）；INFN - Laboratori Nazionali del Gran Sasso（格兰萨索国家实验室）；Dipartimento di Scienze Fisiche e Chimiche, Università degli Studi dell’Aquila（阿奎拉大学物理与化学系）
New Constraints on Cosmic-ray boosted Sub-GeV Dark Matter via Light Mediators
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台暗物质与空间天文重点实验室）；School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
Probing Cosmic-Ray-Boosted and Supernova-Sourced Sub-GeV Dark Matter with Paleo-Detectors
International Centre for Theoretical Physics Asia-Pacific (ICTP-AP), University of Chinese Academy of Sciences（国际理论物理中心亚太分部，中国科学院大学）；Key Laboratory of DM and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（暗物质与空间天文重点实验室，中国科学院紫金山天文台）；School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；Department of Physics and Institute of Theoretical Physics, Nanjing Normal University（南京师范大学物理系和理论物理研究所）
The Cosmic Neutrino Background is within Reach of Future Neutrino Telescopes
Massachusetts Institute of Technology（麻省理工学院）；Harvard University（哈佛大学）；Virginia Tech（弗吉尼亚理工大学）；Institute of Science Tokyo（东京科学大学）；The University of Tokyo（东京大学）
Discriminating Dark Matter Origins with Directional Detection
ARC Centre of Excellence for Dark Matter Particle Physics, School of Physics, The University of Melbourne（墨尔本大学物理学院暗物质粒子物理卓越研究中心）；ARC Centre of Excellence for Dark Matter Particle Physics, School of Physics, The University of Sydney（悉尼大学物理学院暗物质粒子物理卓越研究中心）
