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国际医学放射学杂志 2024年第4期 498-499页

作者： l.p.wang p.wang H.F.Shao J.li Q.l.Yang 高佳音

摘要目的比较对比增强乳腺X线摄影（CEM）与单独低能量成像（lEI）、CEM与MRI对乳腺导管原位癌（DCIS）的术前诊断价值。方法这项单中心回顾性研究分析了术前2

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Capacitance of High-Voltage Coaxial Cable in plasma Immersion Ion Implantation

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Journal of Materials Science & Technology 2001年第1期17卷 41-42页

作者： X.B.Tian l.p.wang D.T.K.Kwok B.Y Tang p.K.Chu Department of physics&Materials Science City University of Hong KongHong KongChina

plasma immersion ion implantation (pIII) is an excellent technique for the surf see modification of complex-shaped components. Owing to pulsed operation mode of the high voltage and large slew rate, the capacitance on the high-voltage coaxial cable can be detrimental to the process and cannot be ignored. In fact, a significant portion of the rise-time/fall-time of the implantation voltage pulse and big initial current can be attributed to the coaxial cable.

关键词： surface modification ion implantation high voltage mode of

Evidence for particle acceleration approaching peV energies in the W51 complex

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Science Bulletin 2024年第18期69卷 2833-2841页

作者： lHAASO Collaboration Zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.J.Bi Y.J.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.X.Chen liang Chen lin Chen long Chen M.J.Chen M.l.Chen Q.H.Chen S.Chen S.H.Chen S.Z.Chen T.l.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.Z.Dai H.l.Dai Z.G.Dai Danzengluobu X.Q.Dong K.K.Duan J.H.Fan Y.Z.Fan J.Fang J.H.Fang K.Fang C.F.Feng H.Feng l.Feng S.H.Feng X.T.Feng Y.Feng Y.l.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge l.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.l.Guo X.l.Guo Y.Q.Guo Y.Y.Guo Y.A.Han M.Hasan H.H.He H.N.He J.Y.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.Huang T.Q.Huang W.J.Huang X.T.Huang X.Y.Huang Y.Huang X.l.Ji H.Y.Jia K.Jia K.Jiang X.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Kuleshov K.Kurinov B.B.li C.M.li Cheng li Cong li D.li F.li H.B.li H.C.li Jian li Jie li K.li S.D.li W.l.li W.l.li X.R.li Xin li Y.Z.li Zhe li Zhuo li E.W.liang Y.F.liang S.J.lin B.liu C.liu D.liu D.B.liu H.liu H.D.liu J.liu J.l.liu M.Y.liu R.Y.liu S.M.liu W.liu Y.liu Y.N.liu Q.luo Y.luo H.K.lv B.Q.Ma l.l.Ma X.H.Ma J.R.Mao Z.Min W.Mitthumsiri H.J.Mu Y.C.Nan A.Neronov l.J.Ou p.pattarakijwanich Z.Y.pei J.C.Qi M.Y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz l.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.X.Sun Q.N.Sun X.N.Sun Z.B.Sun J.Takata p.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian C.wang C.B.wang G.W.wang H.G.wang H.H.wang J.C.wang Kai wang Kai wang l.p.wang l.Y.wang p.H.wang R.wang W.wang X.G.wang X.Y.wang Y.wang Y.D.wang Y.J.wang Z.H.wang Z.X.wang Zhen wang Zheng wang D.M.Wei J.J.Wei Y.J.Wei T.Wen C.Y.Wu H.R.Wu Q.W.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi J.Xia G.M.Xiang D.X.Xiao G.Xiao Y.l.Xin Y.Xing D.R.Xiong Z.Xiong D.l.Xu R.F.Xu R.X.Xu W.l.Xu l.Xue D.H.Yan J.Z.Yan T.Yan C.W.Yang C.Y.Yang F.Yang F.F.Yang l.l.Yang M.J.Yang R.Z.Yang W.X.Yang Y.H.Yao Z.G.Yao l.Q.Yin N.Yin X.H.You Z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.Zeng T.X.Zeng W.Zeng M.Zha B.B.Zhang F.Zhang H.Zhang 不详 Key laboratory of particle Astrophysics&Experimental physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-planck-Institut for Nuclear physics P.O.Box 103980Heidelberg 69029Germany School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao lee Institute&School of physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian Academy of Sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of China Hefei 230026China State Key laboratory of particle Detection and Electronics China Key laboratory of Dark Matter and Space Astronomy&Key laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for Astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of physics and Astronomy Yunnan UniversityKunming 650091China Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of physics and Astronomy(Zhuhai)&School of physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China ApC UniversitéParis Cité

Theγ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the large High Altitude Air Shower Observatory(lHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2 to 200 *** lHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-lAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~200 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the peV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

由超拍电子伏特加速器产生的超高能伽马射线气泡

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Science Bulletin 2024年第4期69卷 449-457页

作者： lHAASO Collaboration Zhen Cao Chuandong Gao Cong li Ruo-Yu liu Ruizhi Yang 不详 Key laboratory of particle Astrophyics&Experimental physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China University of Science and Technology of China Hefei 230026China

We report the detection of aγ-ray bubble spanning at least 100deg2 in ultra-high energy(UHE)up to a few peV in the direction of the star-forming region Cygnus X,implying the presence super peVatron(s)accelerating protons to at least 10 peV.A log-parabola form with the photon indexΓ(E)=(2.71±0.02)+(0.11±0.02)×log10(E/10 TeV)is found fitting the gamma-ray energy spectrum of the bubble *** sources,“hot spots”correlated with very massive molecular clouds,and a quasi-spherical amorphousγ-ray emitter with a sharp central brightening are observed in the *** the core of~0.5°,spatially associating with a region containing massive OB association(Cygnus OB2)and a microquasar(Cygnus X-3),as well as previously reported multi-TeV sources,an enhanced concentration of UHEγ-rays is observed with 2 photons at energies above 1 *** general feature of the bubble,the morphology,and the energy spectrum,are reasonably reproduced by the assumption of a particle accelerator in the core,continuously injecting protons into the ambient medium.

关键词： Cosmic rays γ-rays Interstellar medium Star cluster

Optimization of performance of the KM2A full array using the Crab Nebula

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Chinese physics C 2024年第6期48卷 169-178页

作者：曹臻 F.Aharonian 安琪阿西克古白云翔包逸炜 D.Bastieri 毕效军毕玉江蔡金庭曹晴曹文羽曹喆常进常劲帆陈尚明陈恩生陈亮陈林陈龙陈明君陈玛丽陈起辉陈素弘陈天禄陈阳程宁程耀东崔明阳崔树旺崔晓红崔昱东戴本忠代洪亮戴子高单增罗布 D.della Volpe 董绪强段凯凯樊军辉范一中方军方堃冯存峰封莉冯少辉丰晓婷冯有亮 S.Gabici 高博高川东高林青高启高卫高伟康葛茂茂耿利斯 G.Giacinti 龚光华苟全补顾旻皓郭福来郭晓磊郭义庆郭莹莹韩毅昂何会海贺昊宁何佳银何新波何钰 M.Heller 贺远强侯博文侯超侯贤胡红波胡铨胡世聪黄代绘黄天奇黄文俊黄性涛黄晓渊黄勇黄志成季筱璐贾焕玉贾康江琨姜晓巍姜泽军金敏康明铭柯通 D.Kuleshov.K.Kurinov 李兵兵李澄李骢李丹李飞李海波李会财李华阳李军李剑李捷李凯李文龙李文莲李秀荣李昕李一卓李哲黎卓梁恩维梁云峰林苏杰刘冰刘成刘栋刘虎刘海东刘佳刘江来刘金艳刘茂元柳若愚刘四明刘伟刘怡刘以农鲁睿罗晴吕洪魁马伯强马玲玲马欣华毛基荣闵振 W.Mitthumsiri 穆慧君南云程 A.Neronov 区子维庞彬宇 p.pattarakijwanich 裴致远齐孟尧祁业情乔冰强秦家军 D.Ruffolo A.Sáiz D.Semikoz 邵澄宇邵琅 O.Shchegolev 盛祥东舒富文宋慧超 Yu.V.Stenkin V.Stepanov 苏扬孙秦宁孙晓娜孙志斌谭柏轩唐庆文唐泽波田文武王超王昌贝王广威王洪光王惠惠王建成汪凯王利苹王玲玉王培汉王冉王为王祥高王祥玉王阳王玉东王岩谨王忠海王仲翔王振王铮韦大明魏俊杰魏永健文韬吴超勇吴含荣武莎吴雪峰吴雨生席邵强夏捷夏君集项光漫肖迪泫肖刚辛广广辛玉良邢祎熊峥徐东莲徐仁峰徐仁新徐伟立薛良闫大海颜景志颜田杨朝文杨帆杨冯帆杨何文杨佳盈杨莉莉杨明洁杨睿智杨深邦姚玉华姚志国叶一锰尹丽巧尹娜游晓浩游智勇于艳红袁强岳华曾厚敦曾婷轩曾玮查敏张彬彬张丰张海明张恒英张建立张丽霞张力张鹏飞张佩佩张瑞张少博张少如张寿山张潇张笑鹏张云峰张毅张勇赵兵赵静赵雷赵立志赵世平郑福周斌周浩周佳能周猛周平周荣周勋秀祝成光祝凤荣朱辉朱科军左雄 lHAASO Collaboration Key laboratory of particle Astrophyics&Experimental physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China Tianfu Cosmic Ray Research Center Chengdu 610000China Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-planck-Institut for Nuclear physics P.O.Box 10398069029 HeidelbergGermany State Key laboratory of particle Detection and Electronics China University of Science and Technology of China Hefei 230026China School of physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Hebei Normal University Shijiazhuang 050024China Key laboratory of Dark Matter and Space Astronomy&Key laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Tsung-Dao lee Institute&School of physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of physics and Astronomy(Zhuhai)&School of physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(Zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275China School of physics and Astronomy Yunnan UniversityKunming 650091China Département de physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève24 Quai Ernest Ansermet1211 GenevaSwitzerland Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China ApC Universit'e Paris Cit'eCNRS/IN2P3CEA/IRFUObservat

The full array of the large High Altitude Air Shower Observatory(lHAASO)has been in operation since July *** its kilometer-square array(KM2A),we optimized the selection criteria for very high and ultrahigh energyγ-rays using data collected from August 2021 to August 2022,resulting in an improvement in significance of the detection in the Crab Nebula of approximately 15%,compared with that of previous *** the implementation of these new selection criteria,the angular resolution was also significantly improved by approximately 10%at tens of *** aspects of the full KM2A array performance,such as the pointing error,were also calibrated using the Crab *** resulting energy spectrum of the Crab Nebula in the energy range of 10-1000 TeV are well fitted by a log-parabola model,which is consistent with the previous results from lHAASO and other experiments.

关键词： γ-ray Crab Nebula significance

The Metastable Zone Width of Sodium Dichromate Dihydrate

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The Metastable Zone Width of Sodium Dichromate Dihydrate

CT上肿瘤-胸膜关系是周围型实性腺癌临床ⅠA期隐匿性淋巴结转移的危险因素

第十七届全国化学热力学和热分析学术会议

作者： l.p.wang Y.p.Dong J.Y.peng N.J.Dong H.T.Feng W.li Qinghai Institute of Salt lakes Chinese Academy of Sciences University of Chinese Academy of Sciences

Sodium dichromate dihydrate, one of the most important chromate compounds, can be widely used in wood preservation, leather tanning, metal finishing, and refractory.1-3 As a raw material, sodium dichromate dihydrate can also be used for the manufacture of both hexavalent and trivalent chromium products.4-5 The quality of these downstream products depends largely on the purity of sodium dichromate dihydrate. The high quality sodium dichromate dihydrate can be produced from industrial crystallization by operating crystallization conditions within the metastable zone throughout the crystallization process.6-8 Therefore, the investigation of Metastable Zone Width（MSZW） in terms of the separation and purification of sodium dichromate dihydrate is of theoretical and technological importance. In this work, polythermal method was used to determine the solubility and MSZW of sodium dichromate dihydrate, and thus the effects of cooling rate, initial composition on the MSZW have been investigated. In our experiment, five initial compositions of sodium dichromate dihydrate have been prepared and then crystallized at known cooling rates of 55, 45, 35, 25, and 15 K·h-1. The constant stirring rate was 450 rpm. The experimental MSZW data has been showed in Figure 1. It shows that the MSZW of sodium dichromate dihydrate narrows with the increase of initial composition. The reason is that the saturation temperature increases with the increase of initial composition, which improves the diffusion and collision probabilities of solute. As a result, the crystallization point goes ahead, thus the MSZW becomes narrow. However, there is an opposite effect of cooling rate on the MSZW of the sodium dichromate dihydrate. It may be seen from Figure 1 that the MSZW broadens with the increase of cooling rate. It is easy to explain that a higher cooling rate will supply a higher supercooling, which enhance the MSZW of sodium dichromate *** investigate the effect of stirring rates on the M

关键词： Metastable zone width Solubility Crystallization Sodium dichromate dihydrate

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国际医学放射学杂志 2023年第4期 487-488页

作者： C.Z.Zhang l.p.wang X.T.Cai M.F.li D.D.Sun p.wang 冉淑华

摘要目的探讨CT上的肿瘤-胸膜关系是否是周围型实性腺癌临床ⅠA期隐匿性淋巴结转移（OlNM）的危险因素。方法研究共纳入232例病人。肿瘤与胸膜的关系分为4

关键词：

The Coarse l^(p)-Novikov Conjecture and Banach Spaces with property(H)

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Chinese Annals of Mathematics,Series B 2024年第2期45卷 193-220页

作者： Huan wang Qin wang Research Center for Operator Algebras School of Mathematical SciencesEast China Normal UniversityShanghai 200241China Key laboratory of MEA Ministry of Educationand Shanghai Key Laboratory of PMMPEast China Normal UniversityShanghai 200241China

In this paper,for 1<p<∞,the authors show that the coarse l^(p)-Novikov conjecture holds for metric spaces with bounded geometry which are coarsely embeddable into a Banach space with Kasparov-Yu’s property(H).

In this paper,for 1pl^(p)-Novikov conjecture holds for metric spaces with bounded geometry which are coarsely embeddable into a Banach space with Kasparov-Yu’s property(H).

关键词： The coarse l^(p)-Novikov conjecture Banach spaces with property(H) Coarse geometry K-Theory

On the functions of astrocyte-mediated neuronal slow inward currents

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Neural Regeneration Research 2024年第12期19卷 2602-2612页

作者： Balázs pál Department of physiology Faculty of MedicineUniversity of DebrecenDebrecenHungary

Slow inward currents are known as neuronal excitatory currents mediated by glutamate release and activation of neuronal extra synaptic N-met hyl-D-aspartate receptors with the contribution of *** events are significantly slower than the excitatory postsynaptic *** of slow inward currents are determined by seve ral factors including the mechanisms of astrocytic activation and glutamate release,as well as the diffusion pathways from the release site towards the extra synaptic recepto *** are stimulated by neuronal network activity,which in turn excite neurons,forming an astrocyte-neuron feedback *** as a consequence of brain edema,astrocytic swelling can also induce slow inward currents under pathological *** is a growing body of evidence on the roles of slow inward currents on a single neuron or local network *** events often occur in synchro ny on neurons located in the same astrocytic *** synchronization of neuronal excitability,slow inward currents also set synaptic strength via eliciting timing-dependent synaptic *** addition,slow inward currents are also subject to non-synaptic plasticity triggered by long-la sting stimulation of the excitatory *** note,there might be important regionspecific differences in the roles and actions triggering slow inward *** greater networks,the pathophysiological roles of slow inward currents can be better understood than physiological *** inward currents are identified in the pathophysiological background of autism,as slow inward currents drive early hypersynchrony of the neural *** inward currents are significant contributors to paroxysmal depolarizational shifts/interictal *** events are related to epilepsy,but also found in Alzheimer's disease,parkinson's disease,and stroke,leading to the decline of cognitive *** with features overlapping with slow inward currents(excitatory,N-methyl-Dasp

关键词： astrocyte cortical spreading depolarization gliotransmission glutamate neural synchronization NMDA receptor paroxysmal depolarizational shift slow inward current

Electron kinetic effects in back-stimulated Raman scattering bursts driven by broadband laser pulses

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Matter and Radiation at Extremes 2024年第4期9卷 54-67页

作者： Q.K.liu l.Deng Q.wang X.Zhang F.Q.Meng Y.p.wang Y.Q.Gao H.B.Cai S.p.Zhu Graduate School China Academy of Engineering PhysicsBeijing 100088China Institute of Applied physics and Computational Mathematics Beijing 100094China School of Nuclear Science and Technology University of Science and Technology of ChinaHefei 230026China Shanghai Institute of laser plasma Shanghai 201800China HEDpS Center for Applied Physics and TechnologyPeking UniversityBeijing 100871China School of physics Zhejiang UniversityHangzhou 310027China

We examine electron kinetic effects in broadband-laser-driven back-stimulated Raman scattering(BSRS)bursts using particle-in-cell *** bursts occur during the nonlinear stage,causing reflectivity spikes and generating large numbers of hot ***-duration simulations are performed to observe burst events,and a simplified model is developed to eliminate the interference of the broadband laser’s random intensity *** the simplified model,we isolate and characterize the spectrum of electron plasma *** spectrum changes from a sideband structure to a turbulence-like structure during the burst.A significant asymmetry in the spectrum is *** asymmetry is amplified and transferred to electron phase space by high-intensity broadband laser pulses,leading to violent vortex-merging and generation of hot *** proportion of hot electrons increases from 6.76%to 14.7%during a single violent burst *** demonstrate that kinetic effects profoundly influence the BSRS evolution driven by broadband lasers.

关键词： scattering kinetic simplified