We discuss the impact of charged massive particle big bang nucleosynthesis(CBBN) to explore the nature of the reheating of the Universe in the case that a new extremely long-lived charged massive particle(CHAMP) exists. If the mass of the CHAMP is within collider reach and it's lifetime is longer than $10^4$sec, the comparison between the CBBN prediction and observed $^6$Li abundances may indicate nonstandard reheating in the early Universe without relying on details of the decay properties. Even if the CHAMP mass is outside the reach of colliders, the cosmological considerations may provide a nontrivial hint for the existence of such very heavy long-lived CHAMPs from the late Universe if the daughter particles are the dominant component of the present dark matter. We consider a low reheating temperature model as an example of the nonstandard reheating scenarios.
Reheating the FCC: Probing Early Matter Domination with Long-Lived Particles
New York University Abu Dhabi（阿布扎比纽约大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Millennium Institute for Subatomic Physics at the High Energy Frontier (SAPHIR)（高能前沿亚原子物理千年研究所 (SAPHIR)）
Can LLP detectors probe the reheating temperature? A case study of vector dark matter
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Millennium Institute for Subatomic Physics at the High Energy Frontier (SAPHIR)（高能前沿亚原子物理千年研究所 (SAPHIR)）；Hefei University of Technology（合肥工业大学）
Massive Graviton Dark Matter from a Gapped Continuum
Universidad de Granada（格拉纳达大学）；Universitat de Barcelona（巴塞罗那大学）；Institut de Física d’Altes Energies (IFAE)（高能物理研究所）；The Barcelona Institute of Science and Technology (BIST)（巴塞罗那科学与技术学院）
Updated BBN Bounds on Hadronic Injection in the Early Universe: The Gravitino Problem
Universidade Federal do Rio Grande do Norte（北里奥格兰德联邦大学）；International Institute of Physics, Universidade Federal do Rio Grande do Norte（北里奥格兰德联邦大学国际物理研究所）；Millennium Institute for Subatomic Physics at the High-Energy Frontier (SAPHIR) of ANID（智利国家研究与创新发展局高能前沿亚原子物理学千年研究所）；Universita degli Studi di Messina（墨西拿大学）；INFN Sezione di Catania（意大利国家核物理研究所卡塔尼亚分部）；Universidad de La Serena（拉塞雷纳大学）
Excitation factors for horizonless compact objects: long-lived modes, echoes, and greybody factors
Dipartimento di Fisica, Sapienza Università di Roma（罗马大学物理系）；INFN, Sezione di Roma（意大利国家核物理研究所罗马分部）；Indian Institute of Technology, Gandhinagar（印度理工学院甘地纳加尔分校）；School of Physical Sciences, Indian Association for the Cultivation of Science（印度科学培养协会物理科学学院）
Decay and lifetime of oscillons coupled to an external scalar field: Insights from instability band analysis
Institute of Science Tokyo（东京科学大学）；Center for Theoretical Physics of the Universe, Institute for Basic Science（基础科学研究院宇宙理论物理中心）；Yonsei University（延世大学）；Tongji University（同济大学）；Institute for Advanced Study of Tongji University（同济大学高等研究院）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo（东京大学前沿研究机构理化学宇宙物质研究所（WPI））；Yangzhou University（扬州大学）
DES16C3cje: A low-luminosity, long-lived supernova
本文介绍了暗能量巡天（DES）观测到的一颗低光度、长寿命的II型超新星（SN II），红移为0.0618。DES16C3cje是唯一的SN。光谱的特征是极窄的光球线对应于非常低的膨胀速度$\lesssim1500$ km s $^{-1}$，并且光变曲线显示了在50天后衰减的初始峰值，然后在另外的100天内缓慢地重新变亮，以达到M $_r\sim -15.5$ mag的绝对亮度。时间光变曲线则慢于由$^{56}$ Co的放射性衰变供电所预期的时间光变曲线，但与由吸积功率所预期的时间光变曲线相当。通过比较测辐射热光变曲线和流体动力学模型，我们发现DES16C3cje可以用以下两种解释：i）低爆炸能量（0.11 foe）和相对较大的$^{56}$ Ni生产0.075 M $_{\odot}$，来自其他SNe II典型的$\sim15$ M $_{\odot}$红超巨星祖先，或ii）相对紧凑的$\sim40$ M $_{\odot}$恒星，爆炸能量为1 foe，和0.08 M $_{\odot}$的$^{56}$ Ni。这两种情况都需要额外的能量输入来解释后期光变曲线，这与以$\sim0.5\times{10^{-8}}$ M $_{\odot}$ s $^{-1}$的速率的回退吸积一致。
