Ignition and increase in Pease limit on current in an ohmically heated high densityZ-pinch

Energetics of an ohmically heated deuterium-tritium high densityZ-pinch has been computed taking into account the energy deposited by the alpha particles produced by fusion. As a result, at higher plasma densities (>10²⁷/m³) and temperatures (>4keV), the pinch current can cross Pease limit and the plasma can get ignited, yielding higher energy gain and neutron yield in a shorter confinement time.     

惯性约束聚变反应速率测量

 聚变反应速率是表征惯性约束聚变热核反应的重要参数,为测量聚变反应速率,研制了一套由闪烁体及鼻锥部分、光学系统和条纹相机组成的测量系统。在神光Ⅲ原型装置上利用新研制的聚变反应速率测量系统进行了聚变反应速率测量。在DT中子产额约为10¹⁰条件下,首次获得了聚变反应速率随时间的变化过程。对影响聚变反应速率测量的相关因素进行详细分析后表明,系统的时间分辨力优于30 ps。     

第一壁材料用纳米结构氧化物弥散强化钢制备工艺及其性能研究进展

近年来发展起来的纳米结构氧化物弥散强化钢(ODS钢),因其有优异的耐高温、抗辐照及力学性能,满足聚变堆第一壁结构材料的要求。本文主要简述了纳米结构ODS钢制备工艺及其性能的研究进展。     

热核聚变实验堆中超导母线绝缘层的红外热波检测

本项研究的目的在于探索热核聚变实验堆中超导母线绝缘层的主动式 红外热波检测方法.文中用装有热水的薄膜袋对预埋脱黏缺陷的试件表面进行接触热激励; 给出了在面热源作用下长圆柱内一维瞬态导热的近似理论模型;通 过对理论模型的模拟和分析,发现对热波降温信号进行微分处理可有效提高缺陷和 非缺陷信号对比度;与闪光灯激励的结果进行比较,显示接触热激励的检测深度优于 闪光灯脉冲热激励.     

受控热核聚变研究及其在我国HT-7超导托卡马克上的最新进展

受控热核聚变研究在发展了50年后，在2003年进入了一个新的阶段，国际热核聚变实验堆项目将最后选址开工。科学工作者们希望这个在新世纪初开始的项目能成为彻底解决能源问题的发端，中国科学院等离子体物理研究所最近在受控热核聚变科研上取得了长足进展，朝着稳态高温等离子体的方向又跨出了坚实的一步．其HT-7超导托卡马克高温等离子体的持续时间达到63．95s，成为目前世界上能开展分钟级高温等离子体放电的仅有的两个超导托卡马克装置之一。文章主要介绍了中国科学院等离子体物理研究所最新的聚变实验研究进展。     

ITER磁体支撑结构有限元分析

磁体支撑结构是国际热核聚变实验反应堆(ITER)的重要部件,对其进行力学特性分析研究是确保整个反应堆正常运行的关键。通过对磁体支撑结构各工况下的强度、刚度的数值分析,给出了磁体支撑结构对应工况下各零部件的应力分布及变形量;分析结果表明磁体支撑结构各零部件的最大应力值均小于许用应力,满足强度要求,各零部件变形合理,不会出现脱开失稳现象。通过数值分析,为国际热核反应堆磁体支撑结构提供了理论设计数据,提升了磁体支撑结构的安全性和可靠性。     

Re-evaluation of the ^23Mg（p,γ） ^24Al reaction rate

Based on a new screening Coulomb model, this paper discusses the effect of electron screening on proton capture reaction of 23Mg. The derived result shows that, in some considerable range of stellar temperatures, the effect of electron screening on resonant reaction is prominent; on the non-resonant reaction the effect is obvious only in the low stellar temperatures. The reaction rates of ^23Mg（p,γ） ^24Al would increase 15%-25% due to the fact that the electron screening are considered in typical temperature range of massive mass white dwarfs, and the results undoubtedly affect the nucleosynthesis of some heavier nuclei in massive mass white dwarfs.     

Multiple focus formation in a Mather gun device

Along with the normally produced pulses of dI/dt, x-ray, optical emission, neutrons and ions by a Mather type plasma focus gun, one more set of pulses were observed to be generated by a low energy device at Trombay, a few 100 ns after the first set of pulses, in majority of the discharges. In a small number of discharges even three or more sets of pulses were observed. Signals from pick-up probes placed in the run down region of the device suggest formation of more than one sheath which subsequently may form more than one focus which in turn is responsible for the second and subsequent sets of pulses.     

恒星氦燃烧关键反应12C(α,γ)16O天体物理S因子及其反应率

恒星氦燃烧阶段3α反应和12C（α,γ）16O反应相互竞争,两者的反应率共同决定了氦燃烧结束后12C与16O的丰度比,该比值是大质量恒星后继演化以及伴随的元素核合成过程的初始条件。目前,氦燃烧12C（α,γ）16O反应起始T₉=0.2处,天体物理模型要求的反应率的精确度要低于10%,然而尚未有实验或理论给出满足要求的结果。最为直接和可靠地获取12C（α,γ）16O反应率的方法,就是尽可能往低能区测量其天体物理S因子,然后通过理论外推到感兴趣的能区。为此基于经典的R-矩阵理论,建立了适用于低能核反应的多道、多能级的约化R-矩阵理论来拟合几乎所有可用的16O系统的实验数据。配合使用协方差统计和误差传播理论,拟合外推得到了客观的、内部自恰的和唯一性好的12C（α,γ）16O反应天体物理S因子。总的外推S因子STOT（0.3 MeV）=162.7±7.3 keV·b,理论上首次给出达到恒星演化与元素核合成模型的最低要求的S因子。基于计算给出的全能区的S因子,数值积分给出了温度位于0.04 6 T₉ 6 10的12C（α,γ）16O天体物理反应率。在T₉=0.2处,推荐的反应率为（7.83 ±0.35）×10-15 cm3mol-1s-1。During stellar helium burning, the rates of 3α and the 12C(α,γ)16O reaction, in competition with one another, determine the relative abundances of 12C and 16O in a massive star. The abundance ratio is the beginning condition of the following nucleosynthesis and star evolution of massive stars, which are extremely sensitive to the rate of 12C(α,γ)16O reaction at T₉=0.2. The most direct and trustworthy way to obtain the reaction rate of the 12C(α,γ)16O reaction is to measure the S factor for that reaction to as low energy as possible, and to extrapolate to energies of astrophysical interest. Based on a new multilevel and multichannel reduced R-matrix theory for applications in nuclear astrophysics, we have obtained an accurate and self-consistent astrophysical S factor of 12C(α,γ)16O, by a global fitting for almost all available experimental data of 16O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of 12C(α,γ)16O was obtained with a recommended value STOT (0.3 MeV)=162.7±7.3 keV·b. And the reaction rates of 12C(α,γ)16O for stellar temperatures between 0.04 6 T₉ 6 10 are provided. At T₉=0.2, the reaction rate is (7.83 ±0.35)×10-15 cm3mol-1s-1, where stellar helium burning occurs.     

Thermonuclear reaction rates from (p,n) reactions

Thermonuclear reaction rates for the temperature range 1≤T ₉≤5 have been extracted from experimentally measured (p, n) cross sections for⁴⁵Sc⁵⁰Ti,⁵¹V,⁵⁴Cr,⁵⁵Mn and⁵⁹Co nuclides below 5 MeV bombarding energy. These reaction rates are important in the build-up of medium and heavy nuclides in the stellar evolution process and nucleosynthesis. To enhance the usefulness of these reaction rates in astrophysical calculations, they have been fitted to an analytic function of temperature, valid throughout the temperature range considered here.