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Energy spectrum of cosmic protons and helium nuclei by a hybrid measurement at 4300 m a.s.l.

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Chinese Physics C 2014年第4期38卷 25-31页

作者： b.bartoli P.bernardini 毕效军 I.bolognino P.branchini A.b.dano A.K.Calabrese Melcarne P.Camarri 曹臻 R.Cardarelli S.Catalanotti 陈松战陈天禄 P.Creti 崔树旺戴木忠 A.d'Amone 单增罗布 I.de Mitri b.d'ettorre piazzoli T.di Girolamo G.di Sciascio 冯存峰冯朝阳冯振勇苟全补郭义庆何会海胡海兵胡红波 M.Iacovacci R.Iuppa 贾焕玉拉巴次仁厉海金 G.Liguori 刘成刘俊刘茂元卢红马玲玲马欣华 G.Mancarella S.M.Mari G.Marsella d.Martello S.Mastroianni P.Montini C.C.Ning M.Panareo b.Panico L.Perrone P.Pistilli F.Ruggieri P.Salvini R.Santonico S.N.Sbano 沈培若盛向东石峰 A.Surdo 谭有恒 P.Vallania S.Vernetto C.Vigorito 王辉吴超勇吴含荣薛良杨群羽杨先楚姚志国袁爱芳查敏张慧敏张力张学尧张勇赵静扎西次仁扎西桑珠周勋秀祝凤荣朱清棋 G.Zizzi 白云翔陈明君陈垚冯少辉高博顾旻皓侯超李晓晓刘佳刘加丽王旭肖刚张丙开张寿山周斌左雄 dipartimento di Fisica dell’Università di Napoli "Federico II" Complesso Universitario di Monte Sant’Angelovia Cinthia Istituto Nazionale di Fisica Nucleare Sezione di Napoli Complesso Universitario di Monte Sant’Angelovia Cinthia dipartimento di Matematica e Fisica "Ennio de Giorgi" Università del Salento via per Arnesano Istituto Nazionale di Fisica Nucleare Sezione di Lecce via per Arnesano Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences dipartimento di Fisica dell’Università di Pavia via Bassi 627100 Pavia Italy Istituto Nazionale di Fisica Nucleare Sezione di Pavia via Bassi 627100 Pavia Italy Istituto Nazionale di Fisica Nucleare Sezione di Roma Tre via della Vasca Navale 8400146 Roma Italy Istituto Nazionale di Fisica Nucleare-CNAF Viale Berti-Pichat 6/240127 Bologna Italy dipartimento di Fisica dell’Università di Roma "Tor Vergata" via della Ricerca Scientifica Istituto Nazionale di Fisica Nucleare Sezione di Roma Tor Vergata via della Ricerca Scientifica Tibet University Hebei Normal University Yunnan University Shandong University Southwest Jiaotong University dipartimento di Fisica dell’Università "Roma Tre" via della Vasca Navale 8400146 Roma Italy Osservatorio Astrofisico di Torino dell’Istituto Nazionale di Astrofisica via P.Giuria 110125 Torino Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino via P.Giuria 110125 Torino Italy dipartimento di Fisica dell’Università di Torino via P.Giuria 110125 Torino Italy Physics department Kunming University Normal College of Fuyang

The energy spectrum of cosmic Hydrogen and Helium nuclei has been measured below the so-called ＂knee＂ by using a hybrid experiment with a wide field-of-view Cherenkov telescope and the Resistive Plate Chamber （RPC） array of the ARGO-YbJ experiment at 4300 m above sea level. The Hydrogen and Helium nuclei have been well separated from other cosmic ray components by using a multi-parameter technique. A highly uniform energy resolution of about 25% is achieved throughout the whole energy range （100-700 TeV）. The observed energy spectrum is compatible with a single power law with index γ=-2.63±0.06.

关键词： Cherenkov telescope ARGO-YbJ energy spectrum hybrid measurement composition

羊八井50m^2RPC地毯性能研究YbJ-ARGO合作组(英文)

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高能物理与核物理 2001年第1期25卷 79-85页

作者：何会海 C.bacci 包克智 F.barone b.bartoli P.bernardini S.bussino E. Calloni R. Cardarelli S.Catalanotti S.Cavaliere F.Cesaroni 查敏 P.Creti 单增罗布 b.d'ettorre piazzoli M.deVincenzi T.diGirolamo G.diSciascio 冯振勇傅宇高晓宇庚庆喜郭宏伟何瑁黄庆 M.I 中国科学院高能物理研究所宇宙线和高能天体物理开放实验室 INFN and dipartimento di Fisica dell’ Universtià di Roma Tre 郑州大学物理系 INFN and dipartimento di Fisica dell'Università di Napoli INFN and dipartimento di Fisica dell'Università di Lecce INFN and dipartimento di Fisica dell’ Universtivà di Roma Tre INFN and dipartimento di Fisica dell'Università di Napoli INFN and dipartimento di Fisica dell'Università di Roma "Tor Verga" INFN and dipartimento di Fisica dell'Università di Lecce 西藏大学数理系拉萨850000 西南交通大学物理系山东大学物理系云南大学物理系西藏大学数理系 Istituto di Cosmogeofisica del CNR and INFN Università della basilicata INFN and dipartimento di Fisica dell'Università di Padova

利用羊八井５０ｍ２ＲＰＣ地毯（ＹＢＪ－ＡＲＧＯ实验原型）的测试数据对其性能进行了分析研究，包括原初粒子方位角分布、天顶角分布、地毯的角分辨、探测时间系统误差对方位角分布的正弦调制、探测时间系统误差的离线修正、几何不对... 详细信息

利用羊八井５０ｍ２ＲＰＣ地毯（ＹＢＪ－ＡＲＧＯ实验原型）的测试数据对其性能进行了分析研究，包括原初粒子方位角分布、天顶角分布、地毯的角分辨、探测时间系统误差对方位角分布的正弦调制、探测时间系统误差的离线修正、几何不对称的小型地毯探测器上原初粒子到达方向重建误差造成的方位角分布的不均匀性等．

关键词： γ射线天文广延大气簇射 RPC 小型地毯探测器

The magnetosheath at high spectral resolution

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Earth and Planetary Physics 2024年第1期8卷 234-246页

作者： K.d.Küntz d.Koutroumpa W.R.dunn A.Foster F.S.Porter d.G.Sibeck b.Walsh The Henry A.Rowland department of Physics and Astronomy Johns Hopkins University3701 San Martin DriveBaltimoreMD21218USA NASA Goddard Space Flight Center 8800 Greenbelt RoadGreenbeltMD 20771USA LATMOS-OVSQ CNRSUVSQ Paris-SaclaySorbonne Université11 Boulevard d’Alembert78280GuyancourtFrance department of Physics and Astronomy University College LondonLondonUK The Centre for Planetary Science at UCL/birkbeck Gower StreetLondon WC1E 6BTUK Center for Astrophysics Harvard University&Smithsonian Institution60 Garden StreetCambridgeMA 02138USA Center for Space Physics Boston University110 Cummington MallBostonMAUSA

While we eagerly anticipate SMILE’s(Solar wind Magnetosphere Ionosphere Link Explorer)unprecedented X-ray observations of the Earth’s magnetosheath and the initiation of a new era of magnetospheric research,it seems appropriate to look ahead to the abilities of the next generation of astrophysics *** these,the Line Emission Mapper(LEM),a large aperture micro-calorimeter based mission,is currently planned to be able to observe the magnetosheath at high spectral resolution(~2 eV).With a field of view of~30′,LEM will allow higher spatial resolution and higher cadence measurement of the motion of a very small portion of the magnetopause over relatively short periods of time(multiple hours),complementing SMILE’s global ***’s strength is its spectral *** will be able to measure the abundance of a broad range of elements and ionization states,many of which are inaccessible to current in situ instruments,and will be able to separate the emission from the magnetosheath from the emission from the cosmic X-ray background using the difference in their relative velocities.

关键词： magnetosheath charge exchange solar wind abundances

Additively manufactured Ti–Ta–Cu alloys for the next-generation load-bearing implants

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International Journal of Extreme Manufacturing 2024年第1期6卷 353-374页

作者： Amit bandyopadhyay Indranath Mitra Sushant Ciliveri Jose d Avila William dernell Stuart b Goodman Susmita bose W.M.Keck biomedical Materials Research Laboratory School of Mechanical and Materials EngineeringWashington State UniversityPullmanWA 99164United States of America Veterinary Clinical Sciences College of Veterinary MedicineWashington State UniversityPullmanWA 99164United States of America department of Orthopedic Surgery Stanford University Medical CenterRedwood CityCA 94063United States of America

bacterial colonization of orthopedic implants is one of the leading causes of failure and clinical complexities for load-bearing metallic implants. Topical or systemic administration of antibiotics may not offer the most efficient defense against colonization, especially in the case of secondary infection, leading to surgical removal of implants and in some cases even limbs. In this study, laser powder b.d fusion was implemented to fabricate Ti3Al2V alloy by a 1:1 weight mixture of CpTi and Ti6Al4V powders. Ti-Tantalum(Ta)–Copper(Cu) alloys were further analyzed by the addition of Ta and Cu into the Ti3Al2V custom alloy. The biological,mechanical, and tribo-biocorrosion properties of Ti3Al2V alloy were evaluated. A 10 wt.% Ta(10Ta) and 3 wt.% Cu(3Cu) were added to the Ti3Al2V alloy to enhance biocompatibility and impart inherent bacterial resistance. Additively manufactured implants were investigated for resistance against Pseudomonas aeruginosa and Staphylococcus aureus strains of bacteria for up to 48 h. A 3 wt.% Cu addition to Ti3Al2V displayed improved antibacterial efficacy, i.e.78%–86% with respect to CpTi. Mechanical properties for Ti3Al2V–10Ta–3Cu alloy were evaluated, demonstrating excellent fatigue resistance, exceptional shear strength, and improved tribological and tribo-biocorrosion characteristics when compared to Ti6Al4V. In vivo studies using a rat distal femur model revealed improved early-stage osseointegration for alloys with10 wt.% Ta addition compared to CpTi and Ti6Al4V. The 3 wt.% Cu-added compositions displayed biocompatibility and no adverse infammatory response in vivo. Our results establish the Ti3Al2V–10Ta–3Cu alloy’s synergistic effect on improving both in vivo biocompatibility and microbial resistance for the next generation of load-bearing metallic implants.

关键词： Ti6Al4V load-bearing implants additive manufacturing 3d printing antibacterial performance

Chemical-assisted MMP reduction on methane-oil systems:Implications for natural gas injection to enhanced oil recovery

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Petroleum 2024年第1期10卷 101-108页

作者： Mohamed Almobarak Matthew b.Myers Colin d.Wood Yongbing Liu Ali Saeedi Quan Xie discipline of Petroleum Engineering WA School of Mines: Minerals Energy and Chemical Engineering Curtin University Commonwealth Scientific and Industrial Research Organization Curtin University Oil and Gas Innovation Centre Management State Key Laboratory of Oil and Gas Reservoir Geology and Exploitation

Miscible natural gas injection is widely considered as a practical and efficient enhanced oil recovery technique. However, the main challenge in this process is the high minimum miscibility pressure（MMP）between natural gas and crude oil, which limits its application and recovery factor, especially in hightemperature reservoirs. Therefore, we present a novel investigation to quantify the effect of chemicalassisted MMP reduction on the oil recovery factor. Firstly, we measured the interfacial tension（IFT） of the methane-oil system in the presence of chemical or CO2to calculate the MMP reduction at a constant temperature（373K） using the vanishing interfacial tension（VIT） method. Afterwards, we performed three coreflooding experiments to quantify the effect of MMP reduction on the oil recovery factor under different injection *** interfacial tension measurements show that adding a small fraction（1.5 wt%） of the tested surfactant（SOLOTERRA ME-6） achieved 9% of MMP reduction, while adding 20 wt% of CO2to the methane yields 13% of MMP reduction. Then, the coreflooding results highlight the significance of achieving miscibility during gas injection, as the ultimate recovery factor increased from 65.5% under immiscible conditions to 77.2% using chemical-assisted methane, and to 79% using gas mixture after achieving near miscible condition. The results demonstrate the promising potential of the MMP reduction to significantly increase the oil recovery factor during gas injection. Furthermore, these results will likely expand the application envelop of the miscible gas injection, in addition to the environmental benefits of utilizing the produced gas by re-injection/recycling instead of flaring which contributes to reducing the greenhouse gas emissions.

关键词： Gas injection Enhanced oil recovery Miscibility Coreflooding

Observation of the Crab Nebula with LHAASO-KM2A−a performance study

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Chinese Physics C 2021年第2期45卷 518-530页

作者： F.Aharonian Q.An Axikegu L.X.bai Y.X.bai Y.W.bao d.bastieri X.J.bi Y.J.bi H.Cai J.T.Cai Z.Cao J.Chang J.F.Chang X.C.Chang b.M.Chen J.Chen L.Chen M.J.Chen M.L.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.d.Cheng S.W.Cui X.H.Cui Y.d.Cui b.Z.dai H.L.dai Z.G.dai d.della Volpe b.d'ettorre piazzoli X.J.dong J.H.Fan Y.Z.Fan Z.X.Fan J.Fang K.Fang C.F.Feng L.Feng S.H.Feng Y.L.Feng b.Gao C.d.Gao Q.Gao W.Gao M.M.Ge L.S.Geng G.H.Gong Q.b.Gou M.H.Gu J.G.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He J.C.He S.L.He X.b.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.b.Hu S.Hu S.C.Hu X.J.Hu d.H.Huang Q.L.Huang W.H.Huang X.T.Huang Z.C.Huang F.Ji X.L.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin d.Kuleshov K.Levochkin b.b.Li C.Li F.Li H.b.Li H.C.Li H.Y.Li J.Li K.Li W.L.Li X.Li X.R.Li Y.Li Y.Z.Li Z.Li E.W.Liang Y.F.Liang S.J.Lin b.Liu C.Liu d.Liu H.Liu H.d.Liu J.Liu J.L.Liu J.S.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.J.Long R.Lu H.K.Lv b.Q.Ma L.L.Ma X.H.Ma J.R.Mao A.Masood W.Mitthumsiri T.Montaruli Y.C.Nan b.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi d.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.d.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun X.N.Sun Z.b.Sun P.H.T.Tam Z.b.Tang W.W.Tian b.d.Wang C.Wang H.Wang H.G.Wang J.C.Wang J.S.Wang L.P.Wang L.Y.Wang R.N.Wang W.Wang X.G.Wang X.J.Wang X.Y.Wang Y.d.Wang Y.J.Wang Y.P.Wang Z.Wang Z.H.Wang Z.X.Wang d.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu S.Wu W.X.Wu X.F.Wu S.Q.Xi J.Xia J.J.Xia G.M.Xiang G.Xiao H.b.Xiao G.G.Xin Y.L.Xin Y.Xing d.L.Xu R.X.Xu L.Xue d.H.Yan C.W.Yang F.F.Yang J.Y.Yang L.L.Yang M.J.Yang R.Z.Yang S.b.Yang Y.H.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.d.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha X.X.Zhai b.b.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.W.Zhang L.Zhang L.X.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Y.Zhang Y.F.Zhang Y.L.Zhang b.Zhao J.Zhao L.Zhao L.Z.Zhao S.P.Zhao F.Zheng Y.Zheng b.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou X.X.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu X.Zuo Key Laboratory of Particle Astrophyics&Experimental Physics division&Computing Center Institute of High Energy PhysicsChinese Academy of Sciences100049 BeijingChina University of Chinese Academy of Sciences 100049 BeijingChina TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key Laboratory of Particle detection and Electronics China University of Science and Technology of China 230026 HefeiAnhuiChina department of Engineering Physics Tsinghua University100084 BeijingChina National Astronomical Observatories Chinese Academy of Sciences100101 BeijingChina National Space Science Center Chinese Academy of Sciences100190 BeijingChina School of Physics Peking University100871 BeijingChina Center for Astrophysics Guangzhou University510006 GuangzhouGuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen University519000 ZhuhaiGuangdongChina School of Physical Science and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina School of Physics and Microelectronics Zhengzhou University450001 ZhengzhouHenanChina School of Astronomy and Space Science Nanjing University210023 NanjingJiangsuChina Key Laboratory of dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210023 NanjingJiangsuChina Institute of Frontier and Interdisciplinary Science Shandong University266237 QingdaoShandongChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences200030 ShanghaiChina Tsung-dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong University200240 ShanghaiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong University610031 ChengduSichuanChina College of Physics Sichuan University610065 ChengduSichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina School of Physics and Tec

A sub-array of the Large High Altitude Air Shower Observatory(LHAASO),KM2A is mainly designed to observe a large fraction of the northern sky to hunt for γ-ray sources at energies above 10 *** though the detector construction is still underway,half of the KM2A array has been operating stably since the end of *** this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy γ-ray *** detect γ-ray signals from the Crab Nebula in both energy ranges of 10-100 TeV and>100 TeV with high significance,by analyzing the KM2A data of 136 live days between december 2019 and May *** the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection *** energy spectrum of the Crab Nebula in the energy range 10-250 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10^(-14).(E/20 TeV)-309±0.06stat±0.02syscm^(-2) s^(-1) TeV^(-1).It is consistent with previous measurements by other *** opens a new window of γ-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be discovered.

关键词： γ-ray Crab Nebula extensive air showers cosmic rays

Prospects for a multi-TeV gamma-ray sky survey with the LHAASO water Cherenkov detector array

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Chinese Physics C 2020年第6期44卷 123-132页

作者： F.Aharonian V.Alekseenko Q.An Axikegu L.X.bai Y.W.bao d.bastieri9 X.J.bi H.Cai Zhe Cao Zhen Cao J.Chang J.F.Chang X.C.Chang S.P.Chao b.M.Chen J.Chen L.Chen L.Chen M.L.Chen M.J.Chen Q.H.Chen S.H.Chen S.Z.Chen T.L.Chen X.L.Chen Y.Chen N.Cheng Y.d.Cheng S.W.Cui X.H.Cui Y.d.Cui b.Z.dai H.L.dai Z.G.dai danzengluobu b.d'ettorre piazzoli J.Fang J.H.Fan Y.Z.Fan C.F Feng L.Feng S.H.Feng Y.L.Feng b.Gao Q.Gao W.Gao M.M.Ge L.S.Geng G.H.Gong Q.b.Gou M.H.Gu Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He J.C.He M.Heller S.L.He Y.He C.Hou d.H.Huang Q.L.Huang W.H.Huang X.T.Huang H.b.Hu S.Hu H.Y.Jia K.Jiang F.Ji C.Jin X.L.Ji K.Levochkin E.W.Liang Y.F Liang Cheng Li Cong Li F.Li H.Li H.b.Li H.C.Li H.M.Li J.Li K.Li W.L.Li X.Li X.R.Li Y.Li Z.Li Z.Li b.Liu C.Liu d.Liu H.d.Liu H.Liu J.Liu J.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.N.Liu Z.X.Liu W.J.Long R.Lu H.K.Lv b.Q.Ma L.L.Ma J.R.Mao A.Masood X.H.Ma W.Mitthumsiri T.Montaruli Y.C.Nan P.Pattarakijwanich Z.Y.Pei b.Q.Qiao M.Y.Qi d.Ruffolo V.Rulev A.Sáiz L.Shao O.Shchegolev X.d.Sheng J.R.Shi Y.Stenkin V.Stepanov Z.b.Sun P.H.T.Tam Z.b.Tang W.W.Tian d.d.Volpe C.Wang H.Wang H.G.Wang J.C.Wang L.Y.Wang W.Wang W.Wang X.G.Wang X.Y.Wang X.J.Wang Y.d.Wang Y.J.Wang Y.N.Wang Y.P.Wang Z.Wang Z.H.Wang Z.X.Wang d.M.Wei J.J.Wei T.Wen C.Y.Wu H.R.Wu S.Wu W.X.Wu X.F.Wu G.M.Xiang G.Xiao G.G.Xin Y.Xing R.X.Xu L.Xue d.H.Yan C.W.Yang F.F.Yang L.L.Yang M.J.Yang R.Z.Yang S.b.Yang Y.H.Yao Z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You Z.Y.You Q.Yuan Y.H.Yu Z.J.Jiang H.d.Zeng T.X.Zeng W.Zeng Z.K.Zeng M.Zha b.b.Zhang H.M.Zhang H.Y.Zhang J.L.Zhang J.W.Zhang L.Zhang P.F.Zhang P.P.Zhang S.R.Zhang S.S.Zhang X.Zhang X.P.Zhang Yi Zhang Yong Zhang Y.F.g Zhang b.Zhao J.Zhao L.Zhao L.Z.Zhao F.Zheng Y.Zheng J.N.Zhou P.Zhou R.Zhou X.X.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu X.Zuo Institute of High Energy Physics Chinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduShichuanChina University of Science and Technology of China 230026 HefeiAnhuiChina Tsinghua University 100084 BeijingChina National Astronomical Observatories Chinese Academy of Sciences100101 BeijingChina National Space Science Center Chinese Academy of Sciences100190 BeijingChina School of Physics Peking University100871 BeijingChina Center for Astrophysics Guangzhou University510006 GuangzhouGuangdongChina Sun Yat-sen University 519000 ZhuhaiGuangdongChina Shool of Physics and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina School of Physics and Engineering Zhengzhou University450001 ZhengzhouHenanChina Nanjing University 210023 NanjingJiangsuChina Key Laboratory of dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210034 NanjingJiangsuChina Institute of Frontier and Interdisciplinary Science Shandong University266237 QingdaoShandongChina Shanghai Astronomical Observatory Chinese Academy of Sciences200030 ShanghaiChina School of Physical Science and Technology Southwest Jiaotong University610031 ChengduSichuanChina Sichuan University 610065 ChengduSichuanChina Key Laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina School of physics and technology Wuhan university430072 WuhanChina Yunnan University 650091 KunmingYunnanChina Yunnan Astronomical Observatories Chinese Academy of Sciences650216 KunmingYunnanChina Institute for Nuclear Research Russian Academy of SciencesMoscowRussia département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde GenéveGenevaSwitzerland department of Physics Faculty of ScienceMahidol UniversityBangkokThailand dublin Institute for Advanced Studies 31 Fitzwilliam PlaceDublin 2Ireland Max-Planc

The Water Cherenkov detector Array(WCdA) is a major component of the Large High Altitude Air Shower Array Observatory(LHAASO), a new generation cosmic-ray experiment with unprecedented sensitivity, currently under construction. WCdA is aimed at the study of TeV γ-rays. In order to evaluate the prospects of searching for TeV γ-ray sources with WCdA, we present a projection of the one-year sensitivity of WCdA to TeV γ-ray sources from TeVCat using an all-sky approach. Out of 128 TeVCat sources observable by WCdA up to a zenith angle of 45°, we estimate that 42 would be detectable in one year of observations at a median energy of 1 TeV. Most of them are Galactic sources, and the extragalactic sources are Active Galactic Nuclei(AGN).

关键词： TeVγ-ray astronomy observational prospect LHAASO-WCdA

Ion heat transport in electron cyclotron resonance heated L-mode plasma on the T-10 tokamak

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Plasma Science and Technology 2024年第4期26卷 52-60页

作者： V.A.KRUPIN M.R.NURGALIEV A.R.NEMETS I.A.ZEMTSOV S.d.SUNTSOV T.b.MYALTON d.S.SERGEEV N.A.SOLOVEV d.V.SARYCHEV d.V.RYJAKOV S.N.TUGARINOV N.N.NAUMENKO National Research Centre“Kurchatov Institute” Moscow 123182Russia bauman Moscow State Technical University Moscow 105005Russia Institution“Project Center ITER” Moscow 123098Russia JSC“SOLAR” Minsk 220034Belarus

Anomalous ion heat transport is analyzed in the T-10 tokamak plasma heated with electron cyclotron resonance heating(ECRH) in second-harmonic extra-ordinary mode. Predictive modeling with empirical scaling for Ohmical heat conductivity shows that in ECRH plasmas the calculated ion temperature could be overestimated, so an increase of anomalous ion heat transport is required. To study this effect two scans are presented: over the EC resonance position and over the ECRH power. The EC resonance position varies from the high-field side to the low-field side by variation of the toroidal magnetic field. The scan over the heating power is presented with on-axis and mixed ECRH regimes. discharges with high anomalous ion heat transport are obtained in all considered regimes. In these discharges the power balance ion heat conductivity exceeds the neoclassical level by up to 10 times. The high ion heat transport regimes are distinguished by three parameters: the ratio Te/Ti, the normalized electron density gradient R/■, and the ion–ion collisionality νii~*. The combination of high Te/Ti, high νii~*, and R/■=6-10 results in values of normalized anomalous ion heat fluxes up to 10 times higher than in the low transport scenario.

关键词： tokamak L-mode electron cyclotron resonance heating ion heat transport

Ferroelectricity Induced by Oxygen Vacancies in Rhombohedral ZrO2 Thin Films

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Energy & Environmental Materials 2024年第1期7卷 233-241页

作者： Veniero Lenzi José P.b.Silva Physics Center of Minho and Porto Universities (CF-UM-UP) University of Minho Laboratory of Physics for Materials and Emergent Technologies Lap METUniversity of Minho National Institute of Materials Physics department of Materials Science and Metallurgy

Rhombohedral phase HfxZr1-xO2（HZO,x from 0 to 1） films are promising for achieving robust ferroelectric polarization without the need for an initial wake-up pre-cycling,as is normally the case for the more commonly ... 详细信息

关键词： charged defects ferroelectric polarization rhombohedral phase stability zirconia