Bremsstrahlung neutrino energy loss for ~(24)Mg, ~(28)Si, ~(32)S, ~(40)Ca, ~(56)Fe in strong electron screening

Based on WeinbergoSalam theory the bremsstrahlung neutrino energy loss for nuclei ~(24)Mg, ~(28)Si, ~(32)S, ~(40)Ca and ~(56)Fe are investigated in strong electron screening. Our results are compared with those of Dicus' and show that the latter are higher by 2 orders of magnitude in the density-temperature region of 10~8 g/cm~3 ≤ρ/μ_e≤10~(11) g/cm~3 and 2.5 ≤ T_9 ≤4.5. On the other hand, the factor C shows that the maximum differences are 99.16%, 99.13%, 99.12%, 99.055%, 99.040% corresponding to the nuclei ~(24)Mg, ~(28)Si, ~(32)S, ~(40)Ca and ~(56)Fe.     

Neutrino energy loss by electron capture on strongly screened iron group nuclei

The influences on the neutrino energy loss rates in iron group nuclei at the same density are investigated in the presence of strong electron screening and in the absence of electron screening. The results show that at a temperature of $15\ti10^9$\,K, the neutrino energy loss rates which come from the electron capture process for most iron group nuclei decrease no more than 2 orders of magnitude but for the others (such as $^{53,55,56,57,58,59,60}$Co, $^{56,59}$Ni) they can decrease about 3 orders of magnitude due to strong electron screening (SES), whereas, at a temperature of $10^9K$ the neutrino energy loss rates of the most iron group nuclei can be diminished greatly due to the SES. For example, $^{61}$Fe, $^{60}$Fe, and $^{62}$Ni the neutrino energy loss rates decrease about 4, 15 and 16 orders of magnitude and for $^{57}$Cr, $^{58}$Cr, and $^{60}$Cr decrease about 18, 12, and 10 orders of magnitude respectively. According to our calculations the neutrino energy loss rates of nuclei $^{58}$Mn, $^{59}$Mn, $^{60}$Mn, and $^{62}$Mn may decrease about 13 orders of magnitude at a temperature of $10^9$\,K due to the SES.     

预-主短脉冲激光驱动的高增益类氖氩软X射线激光

 用数值模拟程序计算了脉宽1.5ps预脉冲和主脉冲激光，经1.2ns的时间延迟先后泵浦喷射的密度为6.632×10^-3g/cm³的氩气柱，以获得高增益的类氖离子电子碰撞激发3p-3s跃迁激光的可能性。结果表明：在等离子体中能够形成宽的类氖离子丰度大于50%的区域，并且具有大于10²⁰ cm^-3的自由电子密度。主脉冲到达之后迅速加热自由电子，高密度的自由电子与类氖离子碰撞激发形成具有很高增益系数的增益区，增益区的半高宽度大约100μm，一维理论计算的增益系数为200~300cm^－1，持续时间大约相当于泵浦激光的时间宽度，在1~2ps之间。     

层子模型中重子的半轻子衰变和高能中微子反应

本文从层子模型的结构观点出发,应用文献[1]中的层子与轻子的弱相互作用等效哈密顿量和文献[2]中给出的(1/2)⁺重子波函数及文献[3]中定出的参数,对(1/2)⁺重子的半轻子衰变和高能中微子的弹性和准弹性反应进行了讨论。文中得到的(1/2)⁺重子的半轻子衰变的理论结果与实验符合较好;得到的ΔS=0过程的轴矢形状因子和ν_μ+n→p+μ^-过程的截面在误差范围内均与实验相符合;得到的ΔS=1过程的轴矢形状因子和ν_μ+p→Λ+μ⁺过程的截面与目前实验给出的粗略结果也是符合的。特别需要指出的是,本文在讨论反应问题时,理论中所包含的参数全部从电磁过程定出,在给出的轴矢形状因子和截面公式中没有引进新的参数。     

Pair neutrino energy loss for nuclei 56Fe at the late stages of stellar evolution

Based on the Weinberg-Salam theory,the pair neutrino energy loss rates for nuclei 56Fe are canvassed for the wide range of density and temperature.The results of ours (QLJ) are compared with those of Beaudet G,Petrosian V and Salpeter E.E's (QBPS),and it shows that the pair neutrino energy loss rates of QBPS are always larger than QLJ .The QBPS is 12.57%,12.86%,14.99%,19.80% times higher than QLJ corresponding to the temperature T9=0.385,1.0,5.0,10,respectively.     

快重离子辐照引起Ni/SiO2界面原子混合及相变研究

在室温下用308 MeV的Xe离子和853 MeV的Pb离子辐照Ni/SiO2样品, 用卢瑟福背散射和X射线衍射技术对样品进行了分析。 通过分析Ni/SiO2样品中元素成分分布和结构随离子辐照剂量和电子能损的变化, 探索了离子辐照在Ni/SiO2样品中引起的界面原子混合与结构相变现象。 实验结果显示, Xe和Pb离子辐照均能引起明显的Ni原子向SiO2基体的扩散并导致界面附近Ni, Si和O原子的混合。 实验观测到低剂量Xe离子辐照可产生NiSi2相, 而高剂量Xe离子辐照则导致了Ni3Si和NiO相的形成。 根据热峰模型, Ni原子的扩散和新相的形成可能由沿离子入射路径强电子激发引起的瞬间热峰过程驱动。Ni/SiO2 interface were irradiated at room temperature with 308 MeV Xe ions to 1×1012, 5×1012 Xe/cm2 and 853 MeV Pb ions to 5×1011 Pb/cm2, respectively. These samples were analyzed using Rutherford Backscattering Spectrometry (RBS) and X ray diffraction spectroscopy (XRD), from which the intermixing and phase change were investigated. The obtained results show that both Xe and Pb ions could induce diffusion of Ni atoms to SiO2 substrates and result in intermixing of Ni with SiO2. Furthermore, 1.0×1012 Xe/cm2 irradiation induced the formation of NiSi2 and 5.0×1012 Xe/cm2 irradiation created Ni3Si and NiO phases. The diffusion of Ni atoms and the formation of new phase may be driven by a transient thermal spike process induced by the intense electronic energy loss along the incident ion path.     

金等离子体的荷态分配数的计算

在非局域热动力学平衡(Non-LTE)下,采用类氢近似,计算得出电子密度分别为6.0×10~(20) cm~(-3)、1.4×10~(21) cm~(-3)、1.0×10~(22) cm~(-3)和1.7×10~(22) cm~(-3)的条件下的三体复合、辐射复合、双电子复合系数随电子温度的变化,得出总的复合系数随电子温度的变化关系;结合相关的电离系数得出相应的离子占有数的比,最后,计算出一定电子密度和温度条件下Au~(48+)～Au~(52+)离子的离子丰度,从而得到金等离子体的荷态分配数与电子温度和电子密度的关系.     

低碰撞能下Ne原子对LiH分子转动猝灭的研究

用密耦方法首次研究了Ne原子和LiH分子低能碰撞下的转动猝灭过程.在碰撞能低于10-4cm-1时,弹性截面趋于常数值,非弹性截面随碰撞速度减小线性增加,遵循Wigner定则预言的趋势.对于一个给定的能量,总的猝灭截面是随着初始j的增加而减少的.当能量在0.01~100 cm-1范围内,弹性和非弹性截面均比其它的体系表现出更复杂的振荡行为,这主要是由于体系具有强的各向异性以及它们具有两个吸引阱而造成的.计算表明,在零温极限下,猝灭速率系数达到10-11cm3s-1数量级.当j=7速率系数出现反转结构.     

The competition of neutrino energy loss due to the pair,photo-,plasma process at the late stages of stellar evolution

Based on the Weinberg-Salam theory,the competition of the Neutrino Energy Loss (NEL) rates due to the pair,photo- and plasma process are canvassed.The ratio factor C1,C2 and C3 which correspond the different contributions of the pair,photo- and plasma neutrino process to those of the total NEL rates are accurately taken into account.The ratio factors are very sensitive to the temperature and density.The ratio factor C2 always is lower than the ratio factor C1 and C3.The pair NEL process is the dominant contribution before the crossed point O(C1=C3=0.45) and the plasma NEL process will be the main dominant contribution after the crossed point O.With increasing temperature,the crossed point O will move to the direction of higher density.     

Neutrino energy loss by electron capture in magnetic field at the crusts of neutron stars

Based on the p-f shell model, the effect of strong magnetic field on neutrino energy loss rates by electron capture is investigated. The calculations show that the magnetic field has only a slight effect on the neutrino energy loss rates in the range of 10⁸—10¹³G on the surfaces of most neutron stars. But for some magnetars, the range of the magnetic field is 10¹³—10¹⁸G, and the neutrino energy loss rates are greatly reduced, even by more than four orders of magnitude due to the strong magnetic field.     

7-碘-8-羟基喹啉-5-磺酸体系分光光度法测定水样中铜的含量

研究了7-碘-8-羟基喹啉-5-磺酸与铜(Ⅱ)的显色反应。在pH=5.0Clark-Lubs缓冲介质中,铜(II)与7-碘-8-羟基喹啉-5-磺酸形成黄色络合物,其最大吸收波长位于380nm处,表观摩尔吸光系数为7.35×103L.mol-1.cm-1,铜(II)的含量在0.15—4.5μg/mL范围内符合比耳定律,线性回归方程为A=0.1122x(μg/mL)+0.0079,相关系数0.9999。方法用于合成水样中微量铜的测定,回收率为99%—110%,结果满意。     

Neutrino Energy Loss by Electron Capture on Nucleus ^56Mn, ^56Fe, ^56Co and ^56Ni in Strong Electron Screening

Based on the p-f shell model, the neutrino energy loss rates for nucleus ^56Mn, ^56Fe, ^56Co and ^56Ni in the electron capture process are canvassed in and not in a strong electron screening. The results show that the neutrino energy loss rates for ^56Mn, ^56Fe, ^56Co and ^56Ni decrease about 15%, 10%, 60% and i order of magnitude correspondingly at the temperature T9 = 15 and even debase 2 orders of magnitude at the temperature T9 = 1.     

用液芯光纤研究stokes/anti-stokes拉曼强度比测温

液芯光纤可以使拉曼光谱强度提高103倍。研究了在stokes/anti stokes拉曼光谱强度比测温中如何获得理想测温结果的方法。用长为5.20m、内径为50μm的含C6H6和CCl4混合液体的液芯光纤,获得了高强度CCl4的±218cm-1,±314cm-1和±459cm-1的拉曼光谱。利用各光谱带的stokes与anti stokes的强度比(Is/Ia),确定了液芯光纤所在处的温度。实验结果表明,±459cm-1的强度比的实验值与理论值符合得很好,±218cm-1为较好,±314cm-1稍差一些。从理论和实验两方面总结了拉曼频移、光纤损耗、溶剂效应、仪器响应等对测温结果的影响。     

利用混合介质降低黑腔壁辐射能耗的理论研究

 采用Au-Gd混合介质作腔壁，增大腔壁Rosseland不透明度，降低其辐射能耗是提高黑腔辐射温度的途径之一。利用纯Au和Au-Gd混合介质的Rosseland平均辐射不透明度数据库和多次电离区物态方程加入一维辐射流体力学程序，计算分析了在神光 Ⅱ激光装置产生的黑腔X光辐射能源条件下， Au-Gd混合介质作腔壁对提高黑腔辐射温度的影响，得到了Au-Gd混合介质作腔壁可使黑腔辐射温度提高0.1~0.2MK的结论。     

Neutrino-Pair Bremsstrahlung from a Hot Plasma in the Presence of a Strong Magnetic Field

The stellar energy loss rate due to the production of neutrino pairs by Bremsstrahlung is calculated for neutron stars in the presence of a strong magnetic field (B ? 10¹² G) and the Coulomb field of the positive ions. The calculated energy loss rates are applied to nonrelativistic electrons at low densities ? 10⁵ gm/cm³ and relatively low temperatures T ? 10⁹ K.     

奇异星的冷却

从奇异夸克物质的热力学巨势出发计算了奇异星的组份，得到电子丰度随强相互作用耦合常数或奇异物质的密度增大而减小．利用弱电统一理论，推导了奇异物质的中微子能量损失率。通过研究有薄壳的均匀奇异星和中子垦的冷却过程，得到年轻奇异星的表面温度比同年代的中子星的表面温度低得多，这可以作为区别奇异星与中子星的观测途径。 关键词：     

Constraints and tests of the OPERA superluminal neutrinos

The superluminal neutrinos detected by OPERA indicate Lorentz invariance violation (LIV) of the neutrino sector at the order of 10(-5). We study the implications of the result in this work. We find that such a large LIV implied by OPERA data will make the neutrino production process π → μ + ν(μ) kinematically forbidden for a neutrino energy greater than about 5 GeV. The OPERA detection of neutrinos at 40 GeV can constrain the LIV parameter to be smaller than 3×10(-7). Furthermore, the neutrino decay in the LIV framework will modify the neutrino spectrum greatly. The atmospheric neutrino spectrum measured by the IceCube Collaboration can constrain the LIV parameter to the level of 10(-12). The future detection of astrophysical neutrinos of galactic sources is expected to be able to give an even stronger constraint on the LIV parameter of neutrinos.     

高能激光束在线测量系统的光强衰减设计

针对环形光刀取样式高能激光束在线测量系统应用中光电探测器线性饱和功率密度低而被测高能激光功率密度高的特点,采用对取样激光扩束和介质膜衰减片级联衰减的方式,实现了数千倍的线性光强衰减。介绍了环形光刀扫描取样及其扩束衰减原理,并对介质膜衰减片在激光入射角 0°~15° 和功率密度1~1 000 W/cm2条件下的透过率特性进行了分析,用实验验证了该光强衰减设计的有效性。     

对苯二酚-甲醛碳气凝胶的制备

 溶胶-凝胶法制备了高HC比（10~40,对苯二酚与催化剂(Na₂CO_{3/sub>)的物质的量之比）的对苯二酚-甲醛有机气凝胶,并经高温碳化处理得到其碳气凝胶。借助有机气凝胶的红外光谱研究了其化学结构,说明其网孔结构形成的可能性;研究了有机气凝胶的扫描电镜图像、比表面积及孔径分布等,并得到碳化前后的一些对比数据：有机气凝胶颗粒大小30~50 nm,碳化后约为10 nm,比表面积从341.77 m²/g增大到452.75 m²/g,密度从0.170 8 g/cm^{3/sup>增大到0.335 6 g/cm3/sup>。}}     

Study of beamstrahlung effects at CEPC

The discovery of a 125 GeV Higgs boson at the LHC marked a breakthrough in particle physics. The relative lightness of the new particle has inspired consideration of a high-luminosity Circular Electron Positron Collider(CEPC) as a Higgs Factory to study the particle's properties in an extremely clean environment. Given the high luminosity and high energy of the CEPC, beamstrahlung is one of the most important sources of beaminduced background that might degrade the detector performance. It can introduce even more background to the detector through the consequent electron-positron pair production and hadronic event generation. In this paper,beamstrahlung-induced backgrounds are estimated with both analytical methods and Monte Carlo simulation. Hit density due to detector backgrounds at the first vertex detector layer is found to be~0.2 hits/cm~2 per bunch crossing, resulting in a low detector occupancy below 0.5%. Non-ionizing energy loss(NIEL) and total ionizing dose(TID), representing the radiation damage effects, are estimated to be~10~(11)1 Me V neq/cm~2/yr and~300 k Rad/yr,respectively.