Particle correlation in p+p collision √sNN=200 GeV in PYTHIA

We calculated the relative abundances of charge hadron, K_S⁰, Λ and Λ in the near-side and away-side cones correlated with triggered high p_T particles in minimum bias in p+p collisions at √s_NN=200 GeV in the PYTHIA model. From the quark and gluon jet events in the PYTHIA model, we have found that the particle yields' different splitting. So the di-hadron correlation in the quark jet events and gluon jet events are also presented. And the particle charge dependance of the di-hadron correlation is extracted from the PYTHIA model. The di-hadron plus and di-hadron minus correlations are similar in the near-side (Δφ~0), but in the away-side, the di-hadron minus correlation seems to be lower. The Hadron-K_S⁰ and －Λ+Λ correlations seem to be differet. We have used a double-Gaussian function to fit those correlation functions and compared the fit parameters.     

Electron Scattering by C4H10 and C6H6 in the Energy Range 100--1000eV

We investigate the applicability of the independent atom model （IAM） to elastic electron scattering from complex polyatomic molecules, namely C4H10 and C6H6, in the energy range 100-1000eV. The cross sections of the elastic electron scattering are calculated by employing the IAM together with the relativistic partial waves. The incorporation of both the modified absorption potential and the extended structural factor in the IAM makes the elastic differential cross sections and momentum transfer cross sections have a good agreement with the available experimental data. The present simple model seems to be insensitive to the complexity of the target molecules so that the proposed procedure can be quite useful for calculation of electron scattering from bio-molecules.     

原子核高K同质异能态的诱发γ辐射

介绍了原子核高K同质异能态潜在的应用价值及国内外研究的进展。 总结了形成同质异能态的3种主要物理机制。 说明了高K同质异能态的应用原理是将其激发到更高的不稳定的K混合态上, 再发生诱发退激, 形成γ瀑, 释放其存储的能量。 同时又介绍了K混合态的3种主要产生机制。 最后分析了178Hfm2诱发退变的实验, 讨论了这些实验的区别和与角动量投影壳模型计算结果的差异。The nuclear isomer states have great potential value of application. The important experimental and theoretical researches are presented here. There are three kinds of physics mechanism for the formation of the isomer states. The principle of releasing the energy stored in the isomer is to excite it to higher states, K mixing states, which can spontaneously decay to the ground state forming the γ cascade. After introducting the three ways to form the K mixing states, we analyzed experiments on the most prospective isomer 178Hfm2, discussed the key differences between these experiments and suggested that the Projected Shell Model (PSM) can be helpful to confirm the occurrence of the  K mixing states and would work out characteristics of the induced decay.     

中高能重离子碰撞中的电磁场效应和手征反常现象

重离子碰撞可以产生极强的电磁场和高温高密量子色动力学(QCD)物质,诱导很多重要手征反常现象,例如手征磁效应和手征磁波.本文围绕手征反常现象中的诸多物理要素,详细介绍包括相对论重离子碰撞中不同碰撞系统和能量下的电磁场特性、同质异位素碰撞中寻找手征磁效应、手征磁波特性、中低能重离子碰撞中磁场效应等一系列与电磁场和手征反常现象相关的理论研究成果.相关研究有助于实验中寻找强相互作用中的电荷宇称(CP)破缺的证据,加深对QCD真空涨落和宇宙中正反物质不对称问题的理解.     

中能重离子核反应同位素分布的统计模型计算

用统计擦去模型,引入新的介质中的核子一核子碰撞截面和核物质密度分布弥散度,对中能区由不同质量的重离子引起的核反应的同位素分布进行了研究,探讨了介质效应和核物质密度分布弥散度对同位素分布的影响.     

TMSR白光中子源关键核数据实验进展

钍铀燃料循环核数据的精度和可靠性直接关系着钍基熔盐堆的安全性和经济性。目前大多数核数据都是基于铀钚燃料循环进行开发,若直接用在钍基熔盐堆上将会出现核设计不确定度较高的问题。为了提高钍基熔盐堆物理设计所需核数据的适用性,中国科学院上海应用物理研究所自行设计并建造了紧凑型的15 MeV电子加速器驱动的白光中子源(Photoneutron Source,PNS),用于开展钍铀燃料循环核数据的实验测量。该装置已通过技术验收,并进行了一系列关键核素的核数据测量,检验了现用核数据的可靠性,为相关核素的核数据评价与改进提供了基础实验数据。     

钍基熔盐堆和核能综合利用

发展具有经济可行性、固有安全性且能够更好地解决核燃料和核废料问题的未来先进核能系统,始终是国际核能科技界的努力方向和研发热点,以此为目标,国际核能界在2002年遴选出了六种第四代先进核能系统的候选堆型。钍基熔盐堆是其中唯一的“液态燃料+高温+常压”堆型,其采用氟化熔盐作为核燃料载体或冷却剂,能够在线添加核燃料和处理裂变产物,国际公认适合于钍基核燃料的高效利用。随着技术的进步,被认为是最容易实现商业化的堆型之一。     

Density effect of the neutron halo nucleus induced reactions in intermediate energy heavy ion collisions

Using an isospin-dependent quantum molecular dynamics (IQMD) model, we study the ¹⁵C induced reactions from 30—120 MeV/nucleon systematically. Here the valence neutron of ¹⁵C is assigned at both 1d 5/2 and 2s 1/2 states respectively in order to study the density effect of reaction mechanism. It is believed that the existent neutron halo structure at the 2s 1/2 state of ¹⁵C will affect the light particle emission evidently. In our calculation, the different density distributions of ¹⁵C at two states are calculated by relativistic mean field (RMF) model and introduced in the initiation of IQMD model, respectively. It is found that some observables such as emission fragmentation multiplicity, emission neutron/proton ratio and emission neutrons' kinetic energy spectrum are sensitive to the initial density distribution.     

Temperature dependent fission fragment distribution in the Langevin equation

The temperature dependent width of the fission fragment distributions was simulated in the Langevin equation by taking two-parameter exponential form of the fission fragment mass variance at scission point for each fission event. The result can reproduce experimental data well, and it permits to make reliable estimate for unmeasured product yields near symmetry fission.     

Determination of the stellar reaction rate for 12C（α,γ）16O： using a new expression with the reaction mechanism

The astrophysical reaction rate of 12C(α, γ)16O plays a key role in massive star evolution. However, this reaction rate and its uncertainties have not been well determined yet, especially at T9=0.2. The existing results even disagree with each other to a certain extent. In this paper, the E1, E2 and total (E1+E2) 12C(α, γ)16O reaction rates are calculated in the temperature range from T9=0.3 to 2 according to all the available cross section data. A new analytic expression of the 12 C(α, γ)16 O reaction rate is brought forward based on the reaction mechanism. In this expression, each part embodies the underlying physics of the reaction. Unlike previous works, some physical parameters are chosen from experimental results directly, instead of all the parameters obtained from fitting. These parameters in the new expression, with their 3σ fit errors, are obtained from fit to our calculated reaction rate from T9=0.3 to 2. Using the fit results, the analytic expression of 12C(α, γ)16O reaction rate is extrapolated down to T9=0.05 based on the underlying physics. The 12C(α, γ)16 O reaction rate at T9=0.2 is (8.78 ± 1.52) × 1015 cm3s-1mol-1. Some comparisons and discussions about our new 12 C(α, γ)16 O reaction rate are presented, and the contributions of the reaction rate correspond to the different part of reaction mechanism are given. The agreements of the reaction rate below T9=2 between our results and previous works indicate that our results are reliable, and they could be included in the astrophysical reaction rate network. Furthermore, we believe our method to investigate the 12C(α, γ)16O reaction rate is reasonable, and this method can also be employed to study the reaction rate of other astrophysical reactions. Finally, a new constraint of the supernovae production factor of some isotopes are illustrated according to our 12C(α, γ)16O reaction rates.