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Novel approaches in hadron spectroscopy 强子光谱学的新方法
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-11-01 DOI: 10.1016/j.ppnp.2022.103981
Miguel Albaladejo , Łukasz Bibrzycki , Sebastian M. Dawid , César Fernández-Ramírez , Sergi Gonzàlez-Solís , Astrid N. Hiller Blin , Andrew W. Jackura , Vincent Mathieu , Mikhail Mikhasenko , Victor I. Mokeev , Emilie Passemar , Alessandro Pilloni , Arkaitz Rodas , Jorge A. Silva-Castro , Wyatt A. Smith , Adam P. Szczepaniak , Daniel Winney , (Joint Physics Analysis Center)

The last two decades have witnessed the discovery of a myriad of new and unexpected hadrons. The future holds more surprises for us, thanks to new-generation experiments. Understanding the signals and determining the properties of the states requires a parallel theoretical effort. To make full use of available and forthcoming data, a careful amplitude modeling is required, together with a sound treatment of the statistical uncertainties, and a systematic survey of the model dependencies. We review the contributions made by the Joint Physics Analysis Center to the field of hadron spectroscopy.

在过去的二十年里,无数新的、意想不到的强子被发现。由于新一代的实验,未来会给我们带来更多的惊喜。理解信号和确定状态的性质需要并行的理论努力。为了充分利用现有的和即将到来的数据,需要仔细的振幅建模,同时对统计不确定性进行合理的处理,并对模型依赖性进行系统的调查。综述了联合物理分析中心在强子光谱学领域所作的贡献。
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引用次数: 26
Cosmic nucleosynthesis: A multi-messenger challenge 宇宙核合成:多信使挑战
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-11-01 DOI: 10.1016/j.ppnp.2022.103983
Roland Diehl , Andreas J. Korn , Bruno Leibundgut , Maria Lugaro , Anton Wallner

The origins of the elements and isotopes of cosmic material is a critical aspect of understanding the evolution of the universe. Nucleosynthesis typically requires physical conditions of high temperatures and densities. These are found in the Big Bang, in the interiors of stars, and in explosions with their compressional shocks and high neutrino and neutron fluxes. Many different tools are available to disentangle the composition of cosmic matter, in material of extraterrestrial origins such as cosmic rays, meteorites, stardust grains, lunar and terrestrial sediments, and through astronomical observations across the electromagnetic spectrum. Understanding cosmic abundances and their evolution requires combining such measurements with approaches of astrophysical, nuclear theories and laboratory experiments, and exploiting additional cosmic messengers, such as neutrinos and gravitational waves. Recent years have seen significant progress in almost all these fields; they are presented in this review.

The Sun and the solar system are our reference system for abundances of elements and isotopes. Many direct and indirect methods are employed to establish a refined abundance record from the time when the Sun and the Earth were formed. Indications for nucleosynthesis in the local environment when the Sun was formed are derived from meteoritic material and inclusion of radioactive atoms in deep-sea sediments. Spectroscopy at many wavelengths and the neutrino flux from the hydrogen fusion processes in the Sun have established a refined model of how the nuclear energy production shapes stars. Models are required to explore nuclear fusion of heavier elements. These stellar evolution calculations have been confirmed by observations of nucleosynthesis products in the ejecta of stars and supernovae, as captured by stardust grains and by characteristic lines in spectra seen from these objects. One of the successes has been to directly observe γ rays from radioactive material synthesised in stellar explosions, which fully support the astrophysical models. Another has been the observation of radioactive afterglow and characteristic heavy-element spectrum from a neutron-star merger, confirming the neutron rich environments encountered in such rare explosions. The ejecta material captured by Earth over millions of years in sediments and identified through characteristic radio-isotopes suggests that nearby nucleosynthesis occurred in recent history, with further indications for sites of specific nucleosynthesis. Together with stardust and diffuse γ rays from radioactive ejecta, these help to piece together how cosmic materials are transported in interstellar space and re-cycled into and between generations of stars. Our description of cosmic compositional e

宇宙物质的元素和同位素的起源是理解宇宙演化的一个关键方面。核合成通常需要高温和高密度的物理条件。它们存在于宇宙大爆炸,恒星内部,以及具有压缩激波和高中微子和中子通量的爆炸中。有许多不同的工具可以用来解开宇宙物质的组成,包括宇宙射线、陨石、星尘颗粒、月球和陆地沉积物等地外物质,以及通过电磁频谱的天文观测。了解宇宙丰度及其演化需要将这些测量方法与天体物理学、核理论和实验室实验相结合,并利用其他宇宙信使,如中微子和引力波。近年来,几乎所有这些领域都取得了重大进展;这篇综述介绍了它们。太阳和太阳系是我们元素和同位素丰度的参考系统。许多直接和间接的方法被用来建立一个精确的丰度记录,从太阳和地球形成的时候开始。太阳形成时当地环境中核合成的迹象来自陨石物质和深海沉积物中放射性原子的包裹体。许多波长的光谱学和太阳中氢聚变过程产生的中微子通量建立了一个精细的模型,说明核能的产生是如何塑造恒星的。探索重元素的核聚变需要模型。这些恒星演化的计算已经通过观察恒星和超新星喷出物中的核合成产物得到了证实,这些产物被星尘颗粒捕获,并通过从这些物体中看到的光谱特征线得到了证实。其中一项成功是直接观察到恒星爆炸中合成的放射性物质产生的γ射线,这完全支持了天体物理模型。另一个是对中子星合并的放射性余辉和特征重元素光谱的观察,证实了在这种罕见的爆炸中遇到的富含中子的环境。地球在沉积物中捕获了数百万年的喷出物,并通过特征放射性同位素进行了鉴定,这表明在最近的历史中发生了附近的核合成,并进一步指出了特定核合成的地点。再加上星尘和来自放射性喷射物的弥漫性γ射线,这些有助于拼凑出宇宙物质是如何在星际空间中运输的,以及如何在几代恒星之间再循环的。我们对宇宙成分演化的描述需要这样的观测支持,因为它建立在几个假设之上,而这些假设似乎受到了最近对星系演化过程中常见的剧烈事件的认识的挑战。这篇综述介绍了宇宙物质的流动和核合成的各个地点,这是通过结合许多技术和观察来理解的,朝着目前关于宇宙如何被元素丰富的知识发展。
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引用次数: 10
Holographic approach to compact stars and their binary mergers 致密恒星及其双星合并的全息方法
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-09-01 DOI: 10.1016/j.ppnp.2022.103972
Carlos Hoyos , Niko Jokela , Aleksi Vuorinen

In this review article, we describe the role of holography in deciphering the physics of dense QCD matter, relevant for the description of compact stars and their binary mergers. We review the strengths and limitations of the holographic duality in describing strongly interacting matter at large baryon density, walk the reader through the most important results derived using the holographic approach so far, and highlight a number of outstanding open problems in the field. Finally, we discuss how we foresee holography contributing to compact-star physics in the coming years.

在这篇综述文章中,我们描述了全息术在破译致密QCD物质物理学中的作用,这与描述致密恒星及其双星合并有关。我们回顾了全息二象性在描述大重子密度下强相互作用物质方面的优势和局限性,向读者介绍了迄今为止使用全息方法得出的最重要的结果,并强调了该领域的一些突出的开放问题。最后,我们讨论了我们如何预见全息在未来几年对致密恒星物理学的贡献。
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引用次数: 17
Nuclear weak rates and nuclear weak processes in stars 恒星中的核弱速率和核弱过程
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-09-01 DOI: 10.1016/j.ppnp.2022.103974
Toshio Suzuki

Nuclear weak rates in stellar environments are obtained by taking into account recent advances in shell-model studies of spin-dependent excitation modes in nuclei including Gamow–Teller (GT) and spin-dipole transitions. They are applied to nuclear weak processes in stars such as cooling and heating of the cores of stars and nucleosynthesis in supernovae. The important roles of accurate weak rates for the study of astrophysical processes are pointed out in the following cases. (1) The electron-capture (e-capture) and β-decay rates in sd-shell are evaluated with the USDB Hamiltonian and used to study the evolution of O-Ne-Mg cores in stars with 8–10 M. The important roles of the A = 23 and 25 pairs of nuclei for the cooling of the cores by nuclear Urca processes are investigated. (2) They are also used to study heating of the O-Ne-Mg core by double e-captures on 20Ne in later stages of the evolution. Especially, the e-capture rates for a second-forbidden transition in 20Ne are evaluated with the multipole expansion method by Walecka as well as the method of Behrens–Bühring. Possible important roles of the transition in heating the O-Ne-Mg cores and implications on the final fate of the cores (core-collapse or thermonuclear explosion) are discussed. (3) The weak rates in pf-shell nuclei are evaluated with a new Hamiltonian, GXPF1J, and applied to nucleosynthesis of iron-group elements in Type Ia supernova explosions. The over-production problem of neutron-rich iron isotopes compared with the solar abundances, which remained for the rates according to Fuller, Fowler and Newman, is much improved, and the over-production is now reduced to be within a factor of two. (4) The weak rates for nuclei with two-major shells are evaluated. For sd-pf shell in the island of inversion, the weak rates for the A = 31 pair of nuclei, which are important for nuclear Urca processes in neutron-star crusts, are evaluated with the effective interaction obtained by the extended Kuo–Krenciglowa (EKK) method. Neutron-rich nuclei with and near neutron number (N) of 50 are important for core-collapse processes in supernova explosions. The transition strengths and e-capture rates in 78Ni are evaluated with a new shell-model Hamiltonian for the

恒星环境中的核弱速率是通过考虑原子核中自旋相关激发模式的壳模型研究的最新进展获得的,包括伽莫夫-泰勒(GT)和自旋偶极子跃迁。它们被应用于恒星的核弱过程,如恒星核心的冷却和加热以及超新星的核合成。在下列情况下,指出精确的弱率对研究天体物理过程的重要作用。(1)用USDB哈密顿量计算了sd壳层的电子俘获率和β衰变率,并用于研究8 ~ 10 M⊙恒星中O-Ne-Mg核的演化。研究了A = 23和25对原子核在原子核Urca过程冷却中所起的重要作用。(2)它们也被用来研究在演化后期对20Ne的双e俘获对O-Ne-Mg核的加热。特别地,用Walecka的多极展开法和behrens - b hring法计算了20Ne中第二禁跃迁的电子捕获率。讨论了这种转变在加热O-Ne-Mg核中可能起的重要作用,以及对核的最终命运(核塌缩或热核爆炸)的影响。(3)用新的哈密顿量GXPF1J评价了pf壳核的弱速率,并应用于Ia型超新星爆炸中铁族元素的核合成。富中子铁同位素的生产过剩问题与太阳丰度相比得到了很大的改善,根据富勒、福勒和纽曼的说法,太阳丰度的比率仍然存在,生产过剩的问题现在减少到两倍以内。(4)计算了双主壳核的弱速率。利用扩展的Kuo-Krenciglowa (EKK)方法得到的有效相互作用,对反演岛上的sd-pf壳的A = 31对核的弱速率进行了计算。中子数(N)为50或接近50的富中子核在超新星爆炸的核心坍缩过程中是重要的。利用pf-sdg壳层的新壳层模型哈密顿量计算了78Ni中的跃迁强度和电子捕获速率,并与随机相位近似(RPA)和有效速率公式得到的结果进行了比较。(5)用GT跃迁和第一禁跃迁的壳层模型计算了r过程核合成的等待点核N=126同工核的β衰变率和半衰期。指出了禁止跃迁对质子数(Z)较大的同色同位素的重要作用,发现其半衰期比通过Möller得到的有限范围液滴模型(FRDM)等标准模型得到的半衰期短。(6)用新的壳层模型哈密顿量得到了13C、16O和40Ar上的中微子核反应截面。讨论了对核合成、中微子探测、中微子振荡和中微子质量层次的影响。
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引用次数: 5
Beyond-mean-field approaches for nuclear neutrinoless double beta decay in the standard mechanism 标准机制中核中微子双β衰变的超平均场方法
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-09-01 DOI: 10.1016/j.ppnp.2022.103965
J.M. Yao , J. Meng , Y.F. Niu , P. Ring

Nuclear weak decays provide important probes to fundamental symmetries in nature. A precise description of these processes in atomic nuclei requires comprehensive knowledge on both the strong and weak interactions in the nuclear medium and on the dynamics of quantum many-body systems. In particular, an observation of the hypothetical double beta decay without emission of neutrinos (0νββ) would unambiguously demonstrate the Majorana nature of neutrinos and the existence of the lepton-number-violation process. It would also provide unique information on the ordering and absolute scale of neutrino masses. The next-generation tonne-scale experiments with sensitivity up to 1028 years after a few years of running will probably provide a definite answer to these fundamental questions based on our current knowledge on the nuclear matrix element (NME), the precise determination of which is a challenge to nuclear theory. Beyond-mean-field approaches have been frequently adapted for the study of nuclear structure and decay throughout the nuclear chart for several decades. In this review, we summarize the status of beyond-mean-field calculations of the NMEs of 0νββ decay assuming the standard mechanism of an exchange of light Majorana neutrinos. The challenges and prospects in the extension and application of beyond-mean-field approaches for 0νββ decay are discussed.

核弱衰变为研究自然界的基本对称性提供了重要的途径。要精确地描述原子核中的这些过程,需要对核介质中的强相互作用和弱相互作用以及量子多体系统的动力学有全面的了解。特别是,对假设的双β衰变而不发射中微子(0νββ)的观测将明确地证明中微子的马约拉纳性质和轻子数违反过程的存在。它还将提供关于中微子质量的顺序和绝对尺度的独特信息。基于我们目前对核基质元素(NME)的知识,经过几年的运行,下一代具有高达1028年灵敏度的吨级实验可能会为这些基本问题提供明确的答案,精确确定核基质元素对核理论来说是一个挑战。几十年来,在整个核图中,超平均场方法经常用于核结构和衰变的研究。在这篇综述中,我们总结了假设光马约拉纳中微子交换的标准机制下0νββ衰变的NMEs的超平均场计算的现状。讨论了0νββ衰变的超平均场方法在推广和应用中的挑战和前景。
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引用次数: 20
Coupled-channels calculations for nuclear reactions: From exotic nuclei to superheavy elements 核反应的耦合通道计算:从外来核到超重元素
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-07-01 DOI: 10.1016/j.ppnp.2022.103951
K. Hagino , K. Ogata , A.M. Moro

Atomic nuclei are composite systems, and they may be dynamically excited during nuclear reactions. Such excitations are not only relevant to inelastic scattering but they also affect other reaction processes such as elastic scattering and fusion. The coupled-channels approach is a framework which can describe these reaction processes in a unified manner. It expands the total wave function of the system in terms of the ground and excited states of the colliding nuclei, and solves the coupled Schrödinger equations to obtain the S-matrix, from which several cross sections can be constructed. This approach has been a standard tool to analyze experimental data for nuclear reactions. In this paper, we review the present status and the recent developments of the coupled-channels approach. This includes the microscopic coupled-channels method and its application to cluster physics, the continuum discretized coupled-channels (CDCC) method for breakup reactions, the semi-microscopic approach to heavy-ion subbarrier fusion reactions, the channel coupling effects on nuclear astrophysics and syntheses of superheavy elements, and inclusive breakup and incomplete fusion reactions of weakly-bound nuclei.

原子核是复合系统,在核反应过程中可能受到动态激发。这种激发不仅与非弹性散射有关,而且还影响其他反应过程,如弹性散射和聚变。耦合通道方法是一种可以统一描述这些反应过程的框架。用碰撞核的基态和激发态展开系统的总波函数,求解耦合的Schrödinger方程得到s矩阵,由此可以构造若干截面。这种方法已经成为分析核反应实验数据的标准工具。本文综述了耦合通道方法的研究现状和最新进展。这包括微观耦合通道方法及其在团簇物理中的应用,连续离散耦合通道(CDCC)方法用于分裂反应,半微观方法用于重离子亚势垒聚变反应,通道耦合对核天体物理和超重元素合成的影响,以及弱束缚核的包涵分裂和不完全聚变反应。
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引用次数: 21
Transport model comparison studies of intermediate-energy heavy-ion collisions 中能量重离子碰撞输运模型比较研究
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-07-01 DOI: 10.1016/j.ppnp.2022.103962
Hermann Wolter , Maria Colonna , Dan Cozma , Pawel Danielewicz , Che Ming Ko , Rohit Kumar , Akira Ono , ManYee Betty Tsang , Jun Xu , Ying-Xun Zhang , Elena Bratkovskaya , Zhao-Qing Feng , Theodoros Gaitanos , Arnaud Le Fèvre , Natsumi Ikeno , Youngman Kim , Swagata Mallik , Paolo Napolitani , Dmytro Oliinychenko , Tatsuhiko Ogawa , Wen-Jie Xie

Transport models are the main method to obtain physics information on the nuclear equation of state and in-medium properties of particles from low to relativistic-energy heavy-ion collisions. The Transport Model Evaluation Project (TMEP) has been pursued to test the robustness of transport model predictions in reaching consistent conclusions from the same type of physical model. To this end, calculations under controlled conditions of physical input and set-up were performed with various participating codes. These included both calculations of nuclear matter in a box with periodic boundary conditions, which test separately selected ingredients of a transport code, and more realistic calculations of heavy-ion collisions. Over the years, six studies have been performed within this project. In this intermediate review, we summarize and discuss the present status of the project. We also provide condensed descriptions of the 26 participating codes, which contributed to some part of the project. These include the major codes in use today. After a compact description of the underlying transport approaches, we review the main results of the studies completed so far. They show, that in box calculations the differences between the codes can be well understood and a convergence of the results can be reached. These studies also highlight the systematic differences between the two families of transport codes, known under the names of Boltzmann–Uehling–Uhlenbeck (BUU) and Quantum Molecular Dynamics (QMD) type codes. However, when the codes were compared in full heavy-ion collisions using different physical models, as recently for pion production, they still yielded substantially different results. This calls for further comparisons of heavy-ion collisions with controlled models and of box comparisons of important ingredients, like momentum-dependent fields, which are currently underway. Our evaluation studies often indicate improved strategies in performing transport simulations and thus can provide guidance to code developers. Results of transport simulations of heavy-ion collisions from a given code will have more significance if the code can be validated against benchmark calculations such as the ones summarized in this review.

输运模型是获取低能量到相对论能量重离子碰撞中核态方程和粒子中介质性质物理信息的主要方法。运输模式评估项目(TMEP)旨在检验运输模式预测的稳健性,以从同一类型的物理模式中得出一致的结论。为此,在物理输入和设置的受控条件下,使用各种参与代码进行计算。其中包括在一个具有周期性边界条件的盒子中计算核物质,分别测试传输代码的选定成分,以及更实际的重离子碰撞计算。多年来,在这个项目中进行了六项研究。在这篇中间综述中,我们总结和讨论了项目的现状。我们还提供了26个参与代码的简要描述,它们对项目的某些部分做出了贡献。其中包括目前使用的主要代码。在简要描述了潜在的运输途径之后,我们回顾了迄今为止完成的研究的主要结果。他们表明,在方框计算中,代码之间的差异可以很好地理解,并且可以达到结果的收敛。这些研究还强调了两类传输码之间的系统差异,这两类传输码分别被称为Boltzmann-Uehling-Uhlenbeck (BUU)和量子分子动力学(QMD)类型码。然而,当使用不同的物理模型在完全重离子碰撞中比较这些代码时,就像最近的介子产生一样,它们仍然产生了本质上不同的结果。这就需要用控制模型对重离子碰撞进行进一步的比较,并对重要成分(如动量依赖场)进行盒子比较,目前正在进行中。我们的评估研究经常指出执行传输模拟的改进策略,因此可以为代码开发人员提供指导。如果代码能够通过基准计算(如本文总结的计算)进行验证,那么来自给定代码的重离子碰撞输运模拟结果将具有更大的意义。
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引用次数: 42
Antiprotonic bound systems 反质子束缚系统
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-07-01 DOI: 10.1016/j.ppnp.2022.103964
M. Doser

A wide range of exotic bound systems incorporating antiprotons (atoms, atomic ions, molecules or molecular ions) can be formed, in many cases simply by replacing at least one electron of a matter system by an antiproton. A number of these systems have been studied over decades, while others (in particular antihydrogen) have only recently been the object of precision measurements, and a much larger set have not yet been explored. This review focuses on the physics topics that these exotic systems allow to investigate, and that range from tests of fundamental symmetries to investigating the strong and electromagnetic interactions to probing nuclear models in nuclei far from the line of stability.

在许多情况下,只要用反质子取代物质系统中的至少一个电子,就可以形成包含反质子(原子、原子离子、分子或分子离子)的各种奇异束缚系统。许多这样的系统已经被研究了几十年,而其他的(特别是反氢)直到最近才成为精确测量的对象,更大的一组还没有被探索。这篇综述集中在这些奇异系统允许研究的物理主题上,从基本对称性的测试到研究强相互作用和电磁相互作用,再到在远离稳定线的原子核中探测核模型。
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引用次数: 4
Search for the QCD critical point in high energy nuclear collisions 寻找高能核碰撞中的QCD临界点
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-07-01 DOI: 10.1016/j.ppnp.2022.103960
A. Pandav, D. Mallick, B. Mohanty

QCD critical point is a landmark region in the QCD phase diagram outlined by temperature as a function of baryon chemical potential. To the right of this second-order phase transition point, one expects first order quark–hadron phase transition boundary, towards the left a crossover region, top of it lies the quark–gluon plasma phase and below it the hadronic phase. Hence locating the QCD critical point through relativistic heavy-ion collision experiments is an active area of research. Cumulants of conserved quantities in strong interaction, such as net-baryon, net-charge, and net-strangeness, are suggested to be sensitive to the physics of QCD critical point and are therefore useful observables in the study of the phase transition between quark–gluon plasma and hadronic matter. We review the experimental status of the search for the QCD critical point via the measurements of cumulants of net-particle distributions in heavy-ion collisions. We discuss various experimental challenges and associated corrections in such fluctuation measurements. We also comment on the physics implications of the measurements by comparing them with theoretical calculations. This is followed by a discussion on future experiments and measurements related to high baryonic density QCD matter.

QCD临界点是由温度作为重子化学势的函数所描绘的QCD相图中的一个里程碑区域。在二阶相变点的右边,一阶夸克-强子相变边界,向左是一个交叉区域,它的顶部是夸克-胶子等离子体相,下面是强子相。因此,通过相对论性重离子碰撞实验确定QCD的临界点是一个活跃的研究领域。强相互作用中守恒量的累积量,如净重子、净电荷和净奇异量,被认为对量子cd临界点的物理特性敏感,因此在夸克-胶子等离子体与强子物质之间的相变研究中是有用的观测值。我们回顾了通过测量重离子碰撞中净粒子分布的累积量来寻找QCD临界点的实验现状。我们讨论了这种波动测量中的各种实验挑战和相关修正。我们还通过与理论计算的比较来评论测量的物理含义。随后讨论了未来与高重子密度QCD物质相关的实验和测量。
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引用次数: 11
Corrigendum to “How can Clifford algebra help to understand properties of the second quantized fermions and the corresponding gauge vector and scalar fields” [Prog. Part. Nucl. Phys. 121 (2021) 103890] 《克利福德代数如何帮助理解第二量子化费米子的性质以及相应的规范向量和标量场》的勘误表。部分。诊断。物理学报,121 (2021)103890]
IF 9.6 2区 物理与天体物理 Q1 Physics and Astronomy Pub Date : 2022-07-01 DOI: 10.1016/j.ppnp.2022.103961
N.S. Mankoč Borštnik , H.B. Nielsen
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引用次数: 0
期刊
Progress in Particle and Nuclear Physics
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