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ResearchAccelerator PhysicsTom Katsouleas: use of plasmas as novel particle accelerators and light sources Ying Wu: nonlinear dynamics of charged particle beams, coherent radiation sources, and the development of novel accelerators and light sourcesBiological PhysicsNick Buchler: Molecular mechanisms and the evolution of switches and oscillators in gene networks; systems biology; comparative genomicsGlenn Edwards: Interests include 1) the transduction of light to vibrations to heat and pressure in biological systems and 2) how biology harnesses physical mechanisms during pattern formation in early Drosophila development.Gleb Finkelstein: Electronic transport in carbon nanotubes and graphene; Inorganic nanostructures based on self-assembled DNA scaffolds.Henry Greenside: Theoretical neurobiology in collaboration with Dr. Richard Mooney's experimental group on birdsong.Calvin Howell: Measurement of the neutron-neutron scattering length, carbon and nitrogen accumulation and translocation in plants.Joshua Socolar: Organization and function of complex dynamical networks, especially biological networks, including electronic circuits and social interaction networksWarren Warren: novel pulsed techniques, using controlled radiation fields to alter dynamics; ultrafast laser spectroscopy or nuclear magnetic resonanceCondensed Matter PhysicsHarold Baranger: Theory of quantum phenomena at the nanometer scale;many-body effects in quantum dots and wires; conduction through single molecules; quantum computing; quantum phase transitionsRobert Behringer: Experiments on instabilities and pattern formation in fluids; flow, jamming, and stress patterns in granular materials.David Beratan: molecular underpinnings of energy harvesting and charge transport in biology; the mechanism of solar energy capture and conversion in man-made structuresShailesh Chandrasekharan: Theoretical studies of quantum phase transitions using quantum Monte Carlo methods; lattice QCDAlbert Chang: Experiments on quantum transport at low temperature;one-dimensional superconductivity; dilute magnetic semiconductor quantum dots; Hall probe scanning.Patrick Charbonneau: in- and out-of-equilibrium dynamical properties ofself-assembly. Important phenomena, such as colloidal microphase formation, protein aggregation.Stefano Curtarolo: Nanoscale/microscale computing systems & Quantum Information.Gleb Finkelstein: Experiments on quantum transport at low temperature; carbon nanotubes; Kondo effect; cryogenic scanning microscopy; self-assembled DNA templates.Jianfeng Lu: Mathematical analysis and algorithm development for problems from computational physics, theoretical chemistry, material sciences and others. Maiken H. Mikkelsen: Experiments in Nanophysics & Condensed Matter Physics Richard Palmer: Theoretical models of learning and memory in neural networks; glassy dynamics in random systems with frustrated interactions.Joshua Socolar: Theory of dynamics of complex networks; Modeling of gene regulatory networks; Structure formation in colloidal systems; Tiling theory and nonperiodic long-range order.David Smith: theory, simulation and characterization of unique electromagnetic structures, including photonic crystals and metamaterialsStephen Teitsworth: Experiments on nonlinear dynamics of currents in semiconductors.Weitao Yang: developing methods for quantum mechanical calculations of large systems and carrying out quantum mechanical simulations of biological systems and nanostructuresHigh Energy PhysicsAyana Arce: Searches for top quarks produced in massive particle decays, Jet substructure observable reconstruction, ATLAS detector simulation software frameworkAlfred T. Goshaw: Study of Nature's most massive particles, the W and Z bosons (carriers of the weak force) and the top quark.Ashutosh Kotwal: Experimental elementary particle physics; instrumentation, Precisely measure the mass of the W boson, which is sensitive to the quant um mechanical effects of new particles or forces.Mark Kruse: Higgs boson, production of vector boson pairs, andmodel-independent analysis techniques for new particle searches.Seog Oh: High mass di-lepton search, WW and WZ resonance search, A SUSY particle search, HEP detector R&DKate Scholberg: Experimental particle physics and particle astrophysics; neutrino physics with beam, atmospheric and supernova neutrinos (Super-K, T2K, LBNE, HALO, SNEWS)Chris Walter: Experimental Particle Physics, Neutrino Physics,Particle-Astrophysics, Unification and CP ViolationImaging and Medical PhysicsJames T. Dobbins III: advanced imaging applications to improve diagnostic accuracy in clinical imaging, scientific assessment of image quality, developing lower cost imaging for the developing worldBastian Driehuy: developing and applying hyperpolarized gases to enable fundamentally new applications in MRIAlan Johnson: engineering physics required to extend the resolution of MR imaging and in a broad range of applications in the basic sciencesEhsan Samei: design and utilization of advanced imaging techniques aimed to achieve optimum interpretive, quantitative, and molecular performanceWarren Warren: novel pulsed techniques, using controlled radiation fields to alter dynamics; ultrafast laser spectroscopy or nuclear magnetic resonanceNonlinear and Complex SystemsThe Center for Nonlinear and Complex Systems (CNCS) is an interdisciplinar y University-wide organization that fosters research and teaching of nonlinear dynamics, chaos, pattern formation and complex nonlinear systems with many degrees of freedom.Robert Behringer: Experiments on instabilities and pattern formation in fluids; flow, jamming, and stress patterns in granular materials.Patrick Charbonneau: in- and out-of-equilibrium dynamical properties ofself-assembly. Important phenomena, such as colloidal microphase formation, protein aggregation.Henry Greenside: Theory and simulations of spatiotemporal patterns in fluids; synchronization and correlations in neuronal activity associated with bird song. Daniel Gauthier: Experiments on networks of chaotic elements; generation and control of high speed chaos in electronic and optical systems; electrodynamics of cardiac tissue and the onset of fibrillation.Jian-Guo Liu: Applied mathematics, nonlinear dynamics, complex system, fluid dynamics, computational sciencesRichard Palmer: Theoretical models of learning and memory in neural networks; glassy dynamics in random systems with frustrated interactions.Joshua Socolar: Theory of dynamics of random networks with applications to gene regulation; stress patterns in granular materials; stabilization of periodic orbits in chaotic systems.Stephen Teitsworth: Experiments on nonlinear dynamics of currents in semiconductors.Ying Wu: nonlinear dynamics of charged particle beams, coherent radiation sources, and the development of novel accelerators and light sourcesTom Katsouleas: use of plasmas as novel particle accelerators and light sourcesExperimental Nuclear PhysicsThe Duke physics department is the host of the Triangle Universities Nuclear Laboratory consisting of three experimental facilities: LENA, FN tandem Van de Graff, and The High Intensity Gamma Source (HIGS) at the Free Electron Laser Laboratory.Mohammad Ahmed: Study of few nucleon systems with hadronic and gamma-ray probes.Phillip Barbeau: Experimental Nuclear & Particle Astro-Physics, Double Beta Decay, Neutrinos and Dark MatterHaiyan Gao: Neutron EDM, Precision measurement of proton charge radius, Polarized Compton scattering, neutron and proton transversity, search for phi-N bound state, polarized photodisintegration of 3HeCalvin Howell: quantum chromodynamics (QCD) description of structure and reactions of few-nucleon systems, Big Bang and explosive nucleosynthesis, and applications of nuclear physics in biology, medicine and national security Werner Tornow: weak-interaction physics, especially in double-beta decay studies and in neutrino oscillation physics using large scale detectors at the Kamland project in Japan.Henry Weller: Using radiative capture reactions induced by polarized beams of protons and deuterons to study nuclear systemsYing Wu: nonlinear dynamics of charged particle beams, coherent radiation sources, and the development of novel accelerators and light sourcesTheoretical Nuclear and Particle PhysicsSteffen A. Bass: Physics of the Quark-Gluon-Plasma (QGP) and ultra-relativistic heavy-ion collisions used to create such a QGP under controlled laboratory conditions.Shailesh Chandrasekharan: Quantum Critical Behavior in Fermion Systems, Using the generalized fermion bag algorithm, Applications to Graphene and Unitary Fermi Gas.Thomas Mehen: Quantum Chromodynamics (QCD) and the application of effective field theory to hadronic physics.Berndt Müller: Nuclear matter at extreme energy density; Quantum chromodynamics.Roxanne P. Springer: Weak interactions (the force responsible for nuclear beta decay) and quantum chromodynamics (QCD, the force that binds quarks into hadrons).Geometry and Theoretical PhysicsPaul Aspinwall: String theory is hoped to provide a theory of all fundamental physics encompassing both quantum mechanics and general relativity.Hubert Bray: geometric analysis with applications to general relativity and the large-scale geometry of spacetimes.Ronen Plesser: String Theory, the most ambitious attempt yet at a comprehensive theo ry of the fundamental structure of the universe.Arlie Petters: problems connected to the interplay of gravity and light (gravitational lensing, general relativity, astrophysics, cosmology)Quantum Optics/Ultra-cold atomsDaniel Gauthier: Topics in the fields of nonlinear and quantum optics, and nonlinear dynamical systems.Jungsang Kim: Quantum Information & Integrated Nanoscale SystemsMaiken H. Mikkelsen: Experiments in Nanophysics & Condensed Matter Physics∙Duke University Department of Physics∙Physics Bldg., Science Dr.∙Box 90305∙Durham, NC 27708∙Phone: 919-660-2500∙Fax: 919-660-2525NetID LoginE-Newsletter Sign UpSign up to receive a monthly E-Newsletter or an Annual print Newsletter and keep up with the Physics Department’s scholarly activities∙∙∙∙∙DUKE UNIVERSITY∙GIVING @ DUKE∙WORKING ENVIRONMENT POLICY。
宇宙星辰对应的词1. 太阳 Sun2. 月亮 Moon3. 行星 Planet4. 彗星 Comet5. 伴星 Satellite6. 星系 Galaxy7. 星云 Nebula8. 硬束星 Pulsar9. 中子星 Neutron star10. 黑洞 Black hole11. 银河系 Milky Way12. 外星人 Extraterrestrial13. 陨石 Meteorite14. 陨星 Meteor15. 大爆炸 Big Bang16. 星际尘埃 Interstellar dust17. 行星轨道 Planetary orbit18. 星际空间 Interstellar space19. 红巨星 Red giant20. 白矮星 White dwarf21. 超新星 Supernova22. 恒星 Star23. 恒星演化 Stellar evolution24. 暗物质 Dark matter25. 星际物质 Interstellar matter26. 太阳系 Solar system27. 拉格朗日点 Lagrange point28. 氦闪 Helium flash29. 赤巨星 Red supergiant30. 核融合 Nuclear fusion31. 恒星分类 Stellar classification32. 青年恒星 Young star33. 星际射线 Cosmic ray34. 星际气体 Interstellar gas35. 磁重联 Magnetic reconnection36. 超大质量黑洞 Supermassive black hole37. 恒星表面活动 Stellar surface activity38. 核合成 Nucleosynthesis39. 耀斑 Flare40. 星系群 Galaxy cluster41. 巨星 Giant star42. 行星磁场 Planetary magnetic field43. 行星形成 Planetary formation44. 星际介质 Interstellar medium45. 天文学 Astronomy46. 天体物理学 Astrophysics47. 望远镜 Telescope48. 天文台 Observatory49. 天文学家 Astronomer50. 宇宙学 Cosmology51. 碳星 Carbon star52. 冥王星 Pluto53. 基本粒子 Elementary particle54. 牛顿引力定律 Newton's law of gravitation55. 相对论 Relativity56. 宇宙年龄 Age of the universe57. 宇宙微波背景辐射 Cosmic microwave background radiation58. 珂兹曼定律 Boltzmann's law59. 暗能量 Dark energy60. 探测器 Detector61. 夸克 Quark62. 恒星恒温 Stellar equilibrium temperature63. 双星 Binary star64. 毫秒脉冲星 Millisecond pulsar65. 引力波 Gravitational wave66. 黑洞演化 Black hole evolution67. 星际尘埃云 Interstellar dust cloud68. 行星测量 Planetary measurement69. 宇宙加速膨胀 Cosmic accelerated expansion70. 宇宙红移 Cosmic redshift71. 射电天文学 Radio astronomy72. 中微子 Neutrino73. 超新星遗迹 Supernova remnant74. 星际结构 Interstellar structure75. 行星大气 Planetary atmosphere76. 星际磁场 Interstellar magnetic field77. 恒星形成 Stellar formation78. 能量守恒 Energy conservation79. 暗流 Dark flow80. 毫秒脉冲星双星 Millisecond pulsar binary81. 白矮星新星 White dwarf nova82. 巨星演化 Giant star evolution83. 高能天体物理学 High energy astrophysics84. 统计物理学 Statistical physics85. 背景星 Background star86. 宇宙学中的引力力学 Gravity in cosmology87. 引力透镜 Gravitational lensing88. 行星大气逃逸 Planetary atmospheric escape89. 星际大气 Interstellar atmosphere90. 李普希茨定律 Lippmann's law91. 光谱学 Spectroscopy92. 筛选理论 Selection theory93. 星团 Star cluster94. 星际物质的星际物理学 Interstellar matter in interstellar physics95. 再结晶 Renewal theory96. 镜面反射 Mirror reflection97. 引力微弱 Gravity is weak98. 热核反应 Thermonuclear reaction99. 影响天文学的地球环境 Earth environment affecting astronomy100. 星系和在它们之间移动的物质 Galaxies and matter moving between them。
阿尔茨海默病机制Download tips: This document is carefully compiled by this editor. I hope that after you download it, it can help you solve practical problems. The document can be customized and modified after downloading, please adjust and use it according to actual needs, thank you! In addition, this shop provides you with various types of practical materials, such as educational essays, diary appreciation, sentence excerpts, ancient poems, classic articles, topic composition, work summary, word parsing, copy excerpts, other materials and so on, want to know different data formats and writing methods, please pay attention!阿尔茨海默病（Alzheimer’s disease）是一种慢性进行性神经系统退行性疾病，是老年痴呆的主要形式。
其主要症状包括认知功能受损、记忆障碍、语言障碍、行为异常等，并最终导致患者完全失去自理能力。
目前，阿尔茨海默病的确切机制尚不完全清楚，但研究表明，该疾病可能与多种细胞生物学和神经科学机制有关。
1.β 淀粉样蛋白的异常代谢β淀粉样蛋白是由β-分泌素酶作用于淀粉样前体蛋白产生的多肽，它在健康的大脑中起到抗菌、抗氧化和调节神经元生长的作用。
低强度聚焦超声活化小胶质细胞治疗阿尔茨海默病的动物研究进展李硕1，刘焕亮2，崔慧娟2，曹慧2综述，付源2，3审校摘要：阿尔茨海默病（AD）是老年人群中常见的神经系统变性疾病，以淀粉样斑块异常蓄积为典型病理特征。
血脑屏障因其严格的选择透过性阻止一切大分子物质进入中枢神经系统，成为向脑内输送治疗药物的“瓶颈”。
研究发现，低强度聚焦超声结合超声微泡可通过空化作用安全可逆地打开血脑屏障内皮细胞间隙，并通过促进小胶质细胞向抗炎状态活化减轻淀粉样蛋白沉积。
本综述旨在深入剖析低强度聚焦超声在治疗AD中的最新研究进展，为AD的治疗提供理论基础和新策略。
关键词：阿尔茨海默病；低强度聚焦超声；小胶质细胞；血脑屏障中图分类号：R749.1 文献标识码：AAdvances in animal studies on the activation of microglial cells by low-intensity focused ultrasound in treatment of Alzheimer disease LI Shuo，LIU Huanliang，CUI Huijuan， et al.（Department of Ultrasound， The Fourth Affiliated Hospital of Harbin Medical University， Harbin 150001， China）Abstract：Alzheimer disease is a common neurodegenerative disease among the elderly and has abnormal accumula‑tion of amyloid plaques as the typical pathological feature. Because of its strict selective permeability， the blood-brain bar‑rier prevents all macromolecular substances from entering the central nervous system and has thus become a "bottleneck" for delivering therapeutic drugs to the brain. Studies have shown that low-intensity focused ultrasound combined with ultra‑sound microbubbles can safely and reversibly open the junction between endothelial cells of the blood-brain barrier through cavitation and reduce amyloid deposition by promoting the activation of microglial cells into an anti-inflammatory state. This article reviews the latest research advances in low-intensity focused ultrasound in the treatment of Alzheimer disease，in order to provide a theoretical basis and new strategies for the treatment of Alzheimer disease.Key words：Alzheimer disease；Low‑intensity focused ultrasound；Microglial cell；Blood‑brain barrier阿尔茨海默病（Alzheimer disease，AD）是老年人群中最常见的神经系统变性疾病，其以脑内β淀粉样蛋白（amyloid β-protein，Aβ）异常聚集为典型病理特征，伴随tau蛋白神经原纤维缠结形成及胶质细胞增生密切相关的炎症级联反应等一系列病理改变，最终导致突触丧失及认知功能障碍［1］。
Lesson One 细胞器的结构和功能Actin：肌动蛋白，是微丝的结构蛋白, 以两种形式存在, 即单体和多聚体。
basal body:：基体，真核细胞的纤毛或鞭毛基底部由微管及其相关蛋白质构成的短筒状结构，是纤毛和鞭毛的微管组织中心。
centriole：中心粒，动物、某些藻类和菌类细胞中的圆筒状细胞器，位于间期细胞核附近或有丝分裂细胞的纺锤体极区中心。
chemotaxis：趋化性，即由介质中化学物质的浓度差异形成的刺激所引起的趋向性。
chloroplast：叶绿体，绿色植物细胞内进行光合作用的结构，是一种质体。
chromosome：染色体，实质是脱氧核甘酸，为细胞核内由核蛋白组成、能用碱性染料染色、有结构的线状体，是遗传物质基因的载体。
cilia：纤毛，从一些原核细胞和真核细胞表面伸出的、能运动的突起。
cytoplasm：胞质，由细胞质基质、内膜系统、细胞骨架和包涵物组成。
cytoskeleton：细胞骨架，真核细胞中与保持细胞形态结构和细胞运动有关的纤维网络。
包括微管、微丝和中间丝。
dynein：动力蛋白，即纤毛中的一种具有ATP酶活性的巨大的蛋白质复合体。
endoplasmic reticulum：内质网，指细胞质中一系列囊腔和细管，彼此相通，形成一个隔离于细胞质基质的管道系统。
flagella：鞭毛，在某些细菌菌体上具有细长而弯曲的丝状物，是细菌的运动器官。
Golgi complex：高尔基复合体，由许多扁平的囊泡构成的以分泌为主要功能的细胞器。
lysosome：溶酶体，真核细胞中一种膜包围的异质的消化性细胞器。
是细胞内大分子降解的主要场所。
microfilament：微丝，由肌动蛋白分子螺旋状聚合成的纤丝，又称肌动蛋白丝，是细胞骨架的主要成分之一。
microtubule：微管，由微管蛋白原丝组成的不分支的中空管状结构，是细胞骨架成分，与细胞支持和运动有关。
mitochondrion：线粒体，真核细胞中由双层高度特化的单位膜围成的细胞器。
a r X i v :a s t r o -p h /0307546v 1 31 J u l 2003APS/000-000Neutrino NucleosynthesisA.Heger,1,2E.Kolbe,3W.C.Haxton,nganke,5G.Mart´ınez-Pinedo,6,7and S.E.Woosley 81Department of Astronomy and Astrophysics,The University of Chicago,5640S.Ellis Ave,Chicago,IL 60637,USA 2Theoretical Astrophysics Group,MS B227,Los Alamos National Laboratory,Los Alamos,NM 87545,USA3Departement f¨u r Physik,Universit¨a t Basel,Basel,Switzerland4Institute for Nuclear Theory,University of Washington,Seattle 98195,USA 5Institut for Fysik og Astronomi,˚A rhus Universitet,DK-8000˚A rhus C,Denmark6Institut d’Estudis Espacials de Catalunya,Edifici Nexus,Gran Capit`a 2,E-08034Barcelona,Spain 7Instituci´o Catalana de Recerca i Estudis Avan¸c ats,Llu´ıs Companys 23,E-08010Barcelona,Spain 8Department of Astronomy and Astrophysics,University of California,Santa Cruz,CA95064,USA(Dated:February 2,2008)We study neutrino process nucleosynthesis in massive stars using newly calculated cross sections,an expanded reaction network,and complete and self-consistent models of the progenitor star.We reevaluate the production of light isotopes from abundant progenitors as well as that of rare,heavy,proton-rich isotopes.In particular,new results are given for 11B,19F,138La,and 180Ta.The production of these isotopes places limits on neutrino spectrum and oscialltions.PACS numbers:25.30.Pt,26.20.+f,26.30.+k,26.50.+x,97.60.-s,97.60.BwNuclei can be synthesized in the mantle of a core col-lapse supernova by the neutrino process [1]–energetic supernova neutrinos excite nuclei above particle breakup through neutral-and charge-current reactions,creating new daughter nuclei.While typically only 1%of man-tle nuclei experience inelastic neutrino reactions,certain rare nuclei,one mass unit below abundant parent nuclei such as C,O,and Ne,may nevertheless be produced dominantly by the neutrino process.The final abun-dance depends not only on the instantaneous yield of the daughter isotope,but also whether that isotope survives subsequent processing.In many cases the heating asso-ciated with the passage of the shock destroys the daugh-ter isotope:the surviving nuclei may be only those pro-duced post-shock,after the relevant shell has expanded and cooled.Two recent developments make a re-examination of the ν-process timely.First,we now know about neutrino oscillations,which could alter certain ν-process yields by enhancing charged-current production channels.Sec-ond,new data on the abundances of B and F –two key ν-process products –have been obtained.Prochaska,Howk,and Wolfe [2]recently observed over 25elements in a galaxy at redshift z =2.626,whose young age and high metallicity implies a nucleosynthetic pattern dominated by short-lived,massive stars.Their observation of a so-lar B/O ratio in an approximately 1/3-solar-metallicity gas argues for a primary (metal-independent)production mechanism,such as the ν-process (making 11B),rather than a secondary process,such as cosmic ray proton spal-lation reactions on interstellar CNO seed nuclei (making 10B and 11B).The new F abundance data of Cunha et al.[3]showing a low F/O ratio in two ωCentauri stars argue against AGB-star production of F,and are quite consis-tent with ν-process models (though also with production in cores of stars sufficiently massive to be Wolf-Rayetstars at the beginning of He burning).Until the present effort the most complete neutrino process calculations were those of [4],who evaluated pro-ductions in a 20M ⊙Pop I star evolved without mass loss,including semiconvection,and using the Caughlan et al.[5]12C(α,γ)16O reaction rate.The nuclear chemistry of the coproduced protons and neutrons,which proved to reduce productions of important isotopes like 11B,15N and 19F,was followed in a nuclear reaction network.The effects of shock-wave heating and post-shock neu-trino process production,in shells expanding offthe star and cooling,were ter Timmes et al.[6]extended this calculation to a full galactic model,inte-grating the neutrino process over a range of progenitor stars with evolving metalicity.This letter extends this earlier work in several impor-tant ways.One is the incorporation of mass loss in the evolution of the progenitor star.Second,for the first time a reaction network is employed that includes all of the heavy elements through bismuth using updated reac-tion rates [7]:the work of [4,6]ranged only up to zinc.This allows us to add selected neutrino reactions –the in-clusion of neutrino cross sections for the entire extended network has not yet been attempted –for products that may serve as electron-neutrino ”thermometers.”These cross sections are evaluated in a model that we believe is suitable for heavy nuclei.Third,the nuclear evaporation process –emission of a proton,neutron,or α–is treated in a more sophisticated statistical model that takes into account known nuclear levels and their spins and parities.The various partial neutrino cross sections are calcu-lated as two-step processes,as in [4].The charged-and neutral-current cross sections are evaluated as function of excitation energy in the final nucleus,then a statis-tical model is used to evaluate the subsequent decay by particle or γemission.For the p -and sd -shell nuclei2 the Gamow-Teller(GT)contributions to the(νe,e−)and(ν,ν′)responses were taken from0 ωshell model diag-onalizations,as appropriate.The Cohen-Kurath(14N)[8]and Brown-Wildenthal[9]interactions were used.For12C we adopted energy and GT strength of the main GTtransition,to the T=1state at15.11MeV in12C orits analogue in12N,from experiment.The double-magicnucleus16O has no GT response in the0 ωlimit.Allother contributions to the neutrino cross sections havebeen determined within the random phase approxima-tion(RPA)considering multipoles up to J=4and bothparities.The RPA model,described in[10],treats pro-ton and neutron degrees of freedom separately and em-ploys a partial occupancy formalism for non-closed-shellnuclei.The residual interaction is a zero-range Migdalforce.As realistic shell-model calculations for the heavynuclei(138Ba,139La,181Ta,180Hf)are yet not practical,the entire response was calculated using RPA.In the second step we use the statistical modelSMOKER[11]to calculate,for eachfinal state with well-defined energy,angular momentum,and parity,branch-ing ratios for p,n,αandγemission.SMOKER uses ex-perimentally determined levels in the daughter nucleus,supplemented at higher energies by an appropriate leveldensity formula[11].If the decay leads to an excitedlevel of the daughter nucleus above particle threshold,the subsequent decay of this level is treated similarly.The yield of a given nucleus is obtained by folding thevarious branching ratios,as a function of energy,withthe neutrino response function.This is qualitatively the same procedure used in[4].There full multi-shell shell-model calculations were donethrough16O;in the sd shell,however,thefirst-forbiddenresponse was taken from the simpler Goldhaber-Tellermodel.The sd positive-parity shell model calculationsfor24Mg,28Si,and34S were also truncated.Perhapsmore important,the branching ratios were evaluatedin[4]with a statistical model that lacked the capabili-ties of SMOKER(e.g.,experimental level densities andspin/parity selection rules).In general,the present crosssections turn out to be slightly smaller than those of[4].Detailed partial cross sections for the heavier nu-clei(138Ba,139Ta,180Hf,181Ta)have not been previouslycalculated.For the neutrino spectra we took Fermi-Dirac distri-butions with zero chemical potential and temperaturesT=6MeV forµandτneutrinos and their antiparti-cles and T=4MeV forνe and¯νe.Very recent super-nova simulations[12]find somewhat harderνµ,τspec-tra with T=5.9MeV and a degeneracy parameterα=1.5,predicting slightly larger average neutrino ener-gies and increased cross sections(for example by13%for20Ne(ν,ν′)).The¯νe energies are also found to be moreenergetic than what we assumed,but they have only littleinfluence on the nuclei studied here.Potentially importantν-process candidates can beFIG.1:Dominant neutrino process cross sections for produc-tion for11B,19F,139La,and180Ta as a function of neutrinotemperature(degeneracy parameterα=0).FIG.2:Electron neutrino charged current cross sections on138Ba for cascades up to two particle emission.identified by looking at the abundances in the star dur-ing the explosion,after the passage of the shock.Thisincludes in particular radioactive parent nuclei,existingin nuclear statistical equilibrium or produced in the pas-sage of the shock wave.Table I shows some of the can-didate reactions that were identified from abundancesfound in our progenitor star3.85s after core bounce,the time when the shock reaches the base of the he-lium shell,located at radius4×109cm and mass co-ordinate6.3M⊙.The table includes an estimate of the3 TABLE I:Heavyν-process candidate reactions as derivedform a25M⊙stellar model3.85s after core bounce.σ⊙,42is the cross section in10−42cm2that would be required forsolar production of the isotope.productσ⊙,42parent process11B0.011 1.509 1.899 3.291—–15N0.3960.4800.4860.530—–15M⊙19F0.3750.5770.6430.914—–138La0.1900.2790.974 1.734 2.456180Ta0.599 1.016 2.751 4.628 6.0264 FIG.4:Production of138La in a25M⊙star and its neutrinoprocess progenitor nuclei,139La(neutral current)and138Ba(charged current).The mass fraction of these isotopes as afunction of the enclosed mass is shown before(gray)and after(black)the supernova explosion.TABLE III:Production factor relative to solar normalizedto16O production as a function ofµandτneutrino tem-perature(neutral current)and using4MeV for the electron(ani-)neutrinos(for charged current only).“Hax”are the re-sults from[4]using Haxton’sνcross sections and“Kol”forthe new rates of this paper by Kolbe.productHax Kol Hax Kol Hax Kol Hax 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