双中子星并合的中微子信号

2017年8月17日,LIGO/Virgo首次探测到了双中子星并合事件的引力波信号,随后多波段的跟进观测获得了GW170817事件的多波段“全息”图像并确认源头在40 Mpc外的NGC4993星系,但颇为遗憾的是(尽管与理论预期符合)当时全球运行中的中微子探测器都没有探测到与GW170817相关联的中微子。普遍认为,热中微子在双星引力潮汐撕裂绕行阶段就会产生,在并合事件后的十几毫秒内达到峰值;若并合中心产物为伽马射线暴或者稳定的磁星,还会在并合的即刻至数天内产生超高能中微子。因此,中微子信号不仅可以辅助研究并合后的产物环境,还可以在天文尺度上研究中微子的基本性质和寻找粒子物理标准模型之外的新物理。即使只探测到一个热中微子事件,也可以获得热中微子的能谱标度信息和诊断并合后十几毫秒内星体本身和周围环境的物理参数。另外,因为引力波以光速传播,通过热中微子信号相对引力波信号的时延,可限制中微子的绝对质量。若探测到延迟的高能中微子信号,除了可以清楚地证明双中子星并合的中心产物是磁星,还可以研究并合产物附近的磁场环境和宇宙射线加速机制。     

Neutrino astronomy: Present and future

I briefly review the present and future status of the burgeoning field of neutrino astronomy. I outline the astrophysics and particle physics goals, design, and performance of the various current and proposed neutrino telescopes. Also described are present results and future expectations.     

Space based studies of UHE neutrinos

The Universe at Ultra-High Energies (UHE) above is largely unexplored. In this paper we focus on the search for UHE neutrinos. After briefly summarizing the science rationale for neutrino studies at UHE, we describe the Extreme Universe Space Observatory (EUSO) onboard the Japanese Experiment Module (JEM) of the International Space Station.     

A review of indirect searches for particle dark matter

The indirect detection of dark matter annihilation and decay using observations of photons, charged cosmic rays and neutrinos offers a promising means of identifying the particle nature of this elusive component of the universe. The last decade has seen substantial advances in observational data-sets, complemented by new insights from numerical simulations, which together have enabled for the first time strong constraints on dark matter particle models, and have revealed several intriguing hints of possible signals. This review provides an introduction to indirect detection methods and an overview of recent results in the field.     

宇宙线天体物理中的几个重要问题

宇宙线是来自宇宙空间的高能粒子流,研究宇宙线的起源、加速、传播机制及其所涉及的天体物理和宇宙学过程是宇宙线天体物理研究的重要内容。本文介绍并讨论其中几个涉及物理学一些基本问题的重要课题的研究现状及前景,其中包括极高能宇宙线的观测研究,太阳中微子能谱的实时测量,宇宙线中新粒子的搜寻等。     

Ground-based gamma-ray astronomy: General remarks

Summary The ground-based gamma-ray astronomy has its coming of age currently with 4 sources detected at high significance levels, after experiencing about 30 years history. The energetic gamma rays provide direct means for uncovering higher-energy non-thermal phenomena at various celestial objects. We need more data with improved sensitivities, and multitudes of such efforts are now under way. Paper presented at the Special Session on ground-based gamma-ray astronomy of the XXIV International Cosmic-Ray Conference, Rome, August 28–September 8, 1995.     

揭秘宇宙线起源：LHAASO的使命、挑战与展望

高海拔宇宙线观测站(LHAASO)是人类研究宇宙线最大的实验装置之一,其核心科学目标是寻找宇宙线的起源,不但要探测超高能伽马射线源,也致力于精确测量地球附近带电宇宙线的成分和能谱,系统地研究宇宙线的加速过程及传播机制。从发现12个超高能伽马源(标志着超高能伽马天文学领域的开启),到第一个星表的发布(展现出银河系丰富多彩的宇宙线加速源的候选天体),LHAASO已经为发现宇宙线起源奠定了良好的基础。此外,这些成果为后续的宇宙线加速机理和传播效应的研究指明了方向,同时也为现有理论与模型提供了精确检验的机会与挑战。文章概述了LHAASO项目的开展背景、望远镜主要结构及其在宇宙线物理学中的重大意义,并对其未来的研究方向进行了展望。     

宇宙线天体物理中的几个重要问题

宇宙线是来自宇宙空间的高能粒子流，研究宇宙线的起源、加速、传播机制及其所涉及的天体物理和宇宙学过程是宇宙线天体物理研究的重要内容。本文介绍并讨论其中几个涉及物理学一些基本问题的重要课题的研究现状及前景，其中包括极高能宇宙线的观测研究，太阳中微子能谱的实时测量，宇宙线中新粒子的搜寻等。     

SINGAO: a very large telescope for neutrino gamma astronomy and cosmic-ray studies

Summary We discuss the feasibility of a telescope consisting in a sampling array for extensive air showers measure combined with a muon tracking device. The sampling array will extend over a surface of ≥10⁷ m² while the muon tracking device will cover ≥10⁴ m². The telescope should be done with resistive plates counters and would become a very powerful device to study high-energy neutrinos and gamma-ray astronomy as well as cosmicray physics up to the highest energy (≥10¹⁹ eV) region. The content of this paper has been elaborated with the following people interested in performing the experiment: M. De Palma, G. Iaselli, C. Maggi, S. Natali, S. Nuzzo, A. Ranieri, C. Raso, F. Romano, F. Ruggeri, G. Selvaggi, P. Tempesta, G. Zito; A. Rossi, G. Susinno; A. Grillo, F. Ronga, V. Valente; P. Bernardini, P. Pistilli; A. Watson, R. Reid, M. Lawrence; M. Ambrosio, G. Barbarino, B. Bartoli, V. Silvestrini; R. Buccheri, M. Carollo, O. Catalano, J. Linsley, L. Scarsi; G. Bressi, A. Lanza, M. Cambiaghi, S. Ratti; M. Bonori, G. D'Agostini; M. De Vincenzi, E. Lamanna, P. Lipari, G. Martellotti, F. Massa, M. Mattioli, A. Nigro, S. Petrera; R. Cardarelli, F. Rossi, R. Santonico; L. De Cesare, G. Grella, M. Guida, F. Mancini, G. Marini, G. Romano, G. Vitiello; C. Cappa, B. D'Ettore Piazzoli, P. Ghia, G. Gomez, P. Trivero. [Bari, Cosenza, Laboratori Nazionali di Frascati Lecce, Leeds, Napoli, Palermo, Pavia, Roma I, Roma II, Salerno, Torino, Istituto di Cosmogeofisica del CNR].     

TeV astronomy

With the successful realization of the current-generation of ground-based detectors, TeV Astronomy has entered into a new era. We review recent advances in VHE astronomy, focusing on the potential of Imaging Atmospheric Cherenkov Telescopes （IACTs）, and highlight astrophysical implications of the results obtained within recent years.     

Working group report: Neutrino and astroparticle physics

This is the report of neutrino and astroparticle physics working group at WHEPP-7. Discussions and work on CP violation in long baseline neutrino experiments, ultra high energy neutrinos, supernova neutrinos and water Cerenkov detectors are discussed.     

Probing physics at extreme energies with cosmic ultra-high energy radiation

The highest energy cosmic rays observed possess macroscopic energies and their origin is likely to be associated with the most energetic processes in the universe. Their existence triggered a flurry of theoretical explanations ranging from conventional shock acceleration to particle physics beyond the standard model (SM) and processes taking place at the earliest moments of our universe. Furthermore, many new experimental activities promise a strong increase of statistics at the highest energies and a combination with γ-ray and neutrino astrophysics will put strong constraints on these theoretical models. We give an overview over this quickly evolving research field with focus on testing new particle physics.     

超新星(续)

超新星爆炸是发生在宇宙空间中极为壮观、丰富多彩和引人入胜的重要现象,涉及许多有趣的、尚待探索的物理学研究领域和天体物理学及宇宙学若干相关分支的重要应用.本文试图描述超新星现象研究在各方面的重要意义,提供基本观测事实和理论框架信息以及介绍我们正在从事的部分相关研究工作.     

Significance of the second dip in the ultra-high energy cosmic ray spectrum

A new feature in the spectrum of ultra high energy cosmic rays (UHECR) has been announced in the paper by Berezinsky, Gazizov and Kachelrieβ. The ratio of the solution of the exact transport equation to its solution in the continuous energy loss limit shows intriguing features which, according to the Authors, are related to the very nature of the energy loss processes of UHECR: the very sharp second dip predicted at 6.3 × 10¹⁹ eV can be used as an energy calibration point and also as the UHECR mass indicator for big future cosmic ray experiments. In the present paper we would like to advocate that this statement is an overinterpretation. The second dip is a result of an inappropriate approximation used, and thus it cannot help to understand the nature of UHECR in any way.      

超新星

超新星爆炸是发生在宇宙空间中极为壮观、丰富多彩和引人入胜的重要现象，涉及许多有趣的、尚待探索的物理学研究领域和天体物理学及宇宙学若干相关分支的重要应用．本文试图描述超新星现象研究在各方面的重要意义，提供基本观测事实和理论框架信息以及介绍我们正在从事的部分相关研究工作．     

Twenty years of LUNA

One of the main ingredients of nuclear astrophysics is the knowledge of the thermonuclear reactions responsible for the stellar luminosity and for the synthesis of the chemical elements. Deep underground in the Gran Sasso Laboratory the cross sections of the key reactions of the proton-proton chain and of the Carbon-Nitrogen-Oxygen (CNO) cycle have been measured right down to the energies of astrophysical interest. The main results obtained by LUNA are reviewed, and their influence on the comprehension of the properties of the neutrino and of the Sun are discussed.     

Implications on the origin of cosmic rays in light of 10 TV spectral softenings

Precise measurements of the energy spectra of cosmic rays(CRs)show various kinds of features deviating from single power-laws,which give very interesting and important implications on their origin and propagation.Previous measurements from a few balloon and space experiments indicate the existence of spectral softenings around 10 TV for protons(and probably also for Helium nuclei).Very recently,the DArk Matter Particle Explorer(DAMPE)measurement about the proton spectrum clearly reveals such a softening with a high significance.Here we study the implications of these new measurements,as well as the groundbased indirect measurements,on the origin of CRs.We find that a single component of CRs fails to fit the spectral softening and the air shower experiment data simultaneously.In the framework of multiple components,we discuss two possible scenarios,the multiple source population scenario and the background plus nearby source scenario.Both scenarios give reasonable fits to the wide-band data from TeV to 100 PeV energies.Considering the anisotropy observations,the nearby source model is favored.     

中等银纬区逆康普顿γ射线强度

使用最近期的EGRET/CGRO γ射线数据,确定出了中等银纬区(|b|=10°-20°)银河宇宙线与星际气体相互作用产生的γ射线的发射率q/4π,其中采用了由γ射线数据本身来确定该发射率的方法;并由此获得了以银经为函数的不同能区的逆康普顿(IC)γ射线积分强度.在该银纬区,沿银经平均的IC微分强度可表为:I_Ic(E)=1.58×10^－6E^{－2.08±0.06}cm^－2·s^－1·sr^－1GeV^－1,b=10°—20°;I_Ic(E)=2.08×10^－6E^{－2.03±0.06}cm^－2·s^－1·sr^－1GeV^－1,b=－20°—－10°,其中,能量E的范围为30MeV到4000MeV.