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2023 弥散伽马射线与宇宙线研讨会暨 “宇宙线起源”青年团队年度总结会议

→ Asia/Shanghai
合肥融创美居酒店

合肥融创美居酒店

合肥市万年埠路356号
Qiang Yuan (PMO), Yifeng Wei (University of Science and Technology of China)
Description

宇宙线的起源是一个世纪之谜，研究这一问题需要对宇宙线能谱、各向异性以及伽马射线源和弥散辐射等多信使观测结果。我国的暗物质粒子探测卫星“悟空”号已持续在轨运行7年多时间，在宇宙线粒子能谱直接测量方面取得了系列进展；高海拔宇宙线观测站LHAASO也顺利建成并开始运行，成功开启了拍电子伏特伽马射线观测新窗口。本次会议聚焦于弥散伽马射线与宇宙线实验及理论的新进展，开展专题研讨。

 

研讨会为线下会议，将在合肥巢湖边融创美居酒店内举办。本次研讨会主要为邀请报告模式，也欢迎向组委会提交报告申请。会议不收取注册费，请通过indico会议网页注册并填写酒店需求信息，注册截止日期为10月18日中午12点。

 

会议通知_v2.pdf
合影.jpg
Contact
  • Saturday 21 October
    • 注册
  • Sunday 22 October
    • 1
      Opening/Welcome
    • 青年团队项目: 项目总体进展
      • 2
        青年团队项目总体进展汇报
        Speaker: Qiang Yuan (PMO)
    • Highlight talk
      Convener: Qiang Yuan (PMO)
    • 10:30
      Coffee Break，合影
    • 自由讨论
    • 12:00
      Lunch
    • 弥散伽马观测
      Convener: Guangshun Huang (University of Science and Technology of China)
      • 5
        LHAASO gamma-ray overview
        Speaker: Cong Li
        合肥_2023_10.pdf
      • 6
        LHAASO WCDA diffuse
        Speaker: Peipei Zhang
        LHAASO WCDA diffuse.pdf
      • 7
        Search for VHE Gamma-Rays from the Northern Fermi Bubble with LHAASO

        The Fermi Bubbles are a pair of bubble-like structures symmetric to the galactic center, which are assumed to be morphologically formed by strong energy releasing events happened million years ago. Regarding the emitted Gamma-Rays, high energy radiation processes like hadronic or leptonic emissions accompanying the outflows are responsible for the origin of the emission. As predicted by theoretical works, the difference between hadronic and leptonic emission models locates over TeV bands in the Gamma-Ray spectrum, which is luckily detectable for LHAASO and thus an interesting topic. In this talk, we are going to report the preliminary results on the observed Gamma-Ray flux upper limits with LHAASO-WCDA as well as results from LHAASO-KM2A.

        Speaker: 思达 李 (中国科学院上海天文台)
        SEARCH FOR VHE GAMMA RAYS FROM THE NORTHERN FERMI BUBBLE REGION WITH LHAASO.pptx
      • 8
        DAMPE gamma-ray overview
        Speaker: Zhaoqiang Shen (PMO)
        DAMPE光子进展_弥散辐射会议.pdf
      • 9
        A study of Forbush Decreases effects with DAMPE experiment

        Forbush Decreases (FDs) refer to the rapid decrease and slow recovery in the observed intensity of galactic cosmic rays (GCRs). They are primarily caused by active solar events that sweep low-energy galactic cosmic rays away from Earth. Different characteristics of FDs have been observed through various experiments. The observations are collected mostly from worldwide ground-based Neutron Monitors (NMs). These monitors primarily measure secondary neutrons originating from interactions in the Earth's atmosphere. The Dark Matter Particle Explorer (DAMPE) is a satellite-based cosmic-ray experiment that has been stably opeated for over seven years. Its precise measurements of cosmic ray electrons plus positrons provide a unique perspective for the direct study of FDs. In our analysis, we investigate the properties of FDs observed by DAMPE from 2017 to 2021. These properties include the amplitude of decrease and the recovery time, both as functions of energy. Furthermore, we employ a numerical model to simulate FDs and successfully replicate their process. Our results suggest that head-on CME events lead to energy-dependent recovery times, while edge-on events result in energy-independent recovery times for FDs.

        Speaker: 文昊 李 (中国科学院紫金山天文台)
        Forbush Decrease Analysis_20231022.pdf
    • 16:05
      Coffee Break
    • 弥散伽马理论
      Convener: Fulai Guo (Shanghai Astronomical Observatory, Chinese Academy of Sciences)
      • 10
        Investigating the distribution of cosmic rays using diffuse gamma-rays
        Speaker: Ruizhi Yang
        ruizhi_CR_DISTRIBUTIONS.pdf
      • 11
        On the Origin of Galactic Diffuse TeV-PeY Emission: Insight from LHAASO and IceCube
        Speaker: Kai Yan
        20231021_Hefei_YK.pdf
      • 12
        Multi-messenger Study of Galactic Diffuse Emission with LHAASO and IceCube Observations

        With the breakthrough in PeV gamma-ray astronomy brought by the LHAASO experiment, the high-energy sky is getting richer than before. Lately, LHAASO Collaboration reported the observation of a gamma-ray diffuse emission with energy up to the PeV level from both the inner and outer Galactic plane. In these spectra, there is one bump that is hard to explain by the conventional cosmic-ray transport scenarios. Therefore, we introduce two extra components corresponding to unresolved sources with exponential-cutoff-power-law (ECPL) spectral shape, one with an index of 2.4, and 20 TeV cutoff energy, and another with an index of 2.3 and 2 PeV cutoff energy. With our constructed model, we simulate the Galactic diffuse neutrino flux and find our results are in full agreement with the latest IceCube Galactic plane search. We estimate the Galactic neutrino contributes ∼9% of astrophysical neutrinos at 20 TeV. In the high-energy regime, as expected most of the neutrinos observed by IceCube should be from extragalactic environments.

        Speaker: 苏杰 林 (Sun Yat-Sen University)
        Multi_message_linsj.pptx
      • 13
        宇宙线传播研究进展
        Speaker: Xiaojun Bi
        宇宙线研究.pptx
        宇宙线研究.pptx
    • 18:30
      Social Dinner（融创永乐半山酒店）
  • Monday 23 October
    • 宇宙线直接探测
      Convener: Cheng Liu (IHEP)
    • 10:15
      Coffee Break
    • 宇宙线间接探测
      Convener: Dr Yifeng Wei (University of Science and Technology of China)
    • 12:25
      Lunch
    • 宇宙线理论
      Convener: Chuan Yue
      • 21
        Cosmic Ray Acceleration and Feedback at the Galactic Center
        Speaker: Fulai Guo (Shanghai Astronomical Observatory, Chinese Academy of Sciences)
        hefei23_郭福来.pptx
      • 22
        基于宇宙线多信使反常观测研究其共同起源问题
        Speaker: Yiqing Guo
        宇宙线多信使反常共同起源-2023-中科大.pptx
      • 23
        宇宙线大尺度各向异性起源
        Speaker: Wei Liu
        宇宙线大尺度各向异性起源.pdf
        宇宙线大尺度各向异性起源.pdf
      • 24
        Study of propagation origin of the knee structure in cosmic ray energy spectrum using large-scale anisotropy

        The origin of the knee structure in cosmic ray (CR) energy spectrum remains unresolved. Various types of models have been proposed to explain it, which can be distinguished as acceleration origin (due to the limitation of the maximum possible CR energy by Galactic sources), propagation origin (because of the transition from slow to fast diffusion of Galactic CRs), interaction origin and local source origin. This work focuses on the propagation origin by adopting a double power law rigidity-dependent diffusion coefficient $D(\mathcal{R}) \propto\left\{\begin{array}{c}\mathcal{R}^\delta, \mathcal{R} \leq \mathcal{R}_{\text {knee }} \\ \mathcal{R}^{\delta+\delta_{\text {knee }}, \mathcal{R}>\mathcal{R}_{\text {knee }}}\end{array}\right.$, where $\mathcal{R}_{\text {knee }}$ is the break rigidity and $\delta_{\text {knee }}$ is the index change. By comparing DRAGON calculation with spectra measured by KASCADE, we found $\mathcal{R}_{\text {knee }}\approx1.0\rm{PV}$ and $\delta_{\text {knee }}\approx1.0$. However, giving the above rigidity parameter, the large scale anisotropy observation above 100TeV strongly disfavors this $\delta_{\text {knee }}$ value. Large scale anisotropy suggests that index change is smaller than 0.15 at 95% CL. The propagation origin of the knee is therefore excluded by the anisotropy measurement with a high confidence level.

        Speaker: Hua Yue (Institute of High Energy Physics, CAS)
        岳华knee report 20231023.pptx
      • 25
        Searching for Magnetic Selected UHECR Structures

        The Pierre Auger Observatory (PAO) collaboration has reported more than 2600 ultrahigh-energy cosmic rays (UHECRs) lately. Adopting a universal model with one source and energy-dependent magnetic deflections, we found the magnetic selected UHECR structure from the PAO public data around the direction of Centaurus A.

        Speaker: Haoning He (PMO)
        GRB221009A_1023.pdf
        GRB221009A_1023.pdf
      • 26
        Study of Galactic diffusion coefficient with the spectrum features of UHECR

        The Auger Collaboration has recently published the energy spectrum of cosmic rays above 1 EeV, which exhibits interesting features. These spectrum features provide an opportunity to investigate the propagation of ultra-high-energy cosmic rays (UHECRs). In this study, we have developed a model that incorporates the dip model for UHECRs in the extragalactic propagation, while accounting for the suppression due to diffusion and interactions within the galaxy. Our model demonstrates excellent agreement with the energy spectrum measured by Auger and supports a spectral index of 2 for the diffusion coefficient in the galaxy starting from 5EeV.

        Speaker: Dan li (IHEP)
        李丹Study of Galactic diffusion coefficient with the spectrum features of UHECR.pptx
    • 16:30
      Coffee Break
    • 自由讨论
  • Tuesday 24 October
    • DAMPE实验内部讨论
    • 10:30
      Coffee Break
    • DAMPE实验内部讨论
    • 12:00
      Lunch
    • 自由讨论
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