中子辐射俘获反应机制的质量能量相关性研究

对A?<10?0核质量区内的核素,研究中子辐射俘获反应中不同反应机制对辐射俘获截面的贡献随靶核质量数和中子入射能量变化的规律.所考虑的反应机制有复合核统计过程和复合核弹性散射道中的辐射俘获及形状弹性散射道中的直接–半直接辐射俘获两种非统计过程.在中子入射能量0.1—20MeV区间,给出了²⁷Al,⁴⁰Ca,⁶³Cu和⁹³Nb的理论计算结果及与实验数据的比较,并对呈现的变化规律进行了分析讨论     

197Au中子辐射俘获过程中γ射线强度函数与能谱研究

文章假定在复合核首次和级联γ退激过程中,除包含巨偶极共振模式外,还存在⁶He,⁶Li,⁶Be,⁷Li和⁷Be等粒子集团的激发态的退激过程,并据此建立了包括这些过程的γ射线强度函数,计算了入射中子能量在0.01—3MeV能区的中子辐射俘获反应:¹⁹⁷Au(n,γ)的反应截面和γ能谱,得到了与实验数据较好符合的结果.特别是,很好地解释了γ能谱中5.5MeV之后的反常突起.     

97MeV 16O轰击51V靶出射α粒子的测量与理论分析

用不同种类的粒子望远镜测量了97MeV ¹⁶O+⁵¹V反应中出射的α粒子.得到了单举α粒子能谱、角分布、E-θ平面内的d²σ/dEdΩ截面等高图及速度平面内的d²σ/PCdEdΩ截面等高图.区分了复合核蒸发的α粒子与直接机制发射的α粒子.用激子模型对预平衡发射的α粒子贡献进行估计,得到的预平衡发射和复合核蒸发分别在α粒子总产额中所占的比份.     

光子穿透系数及同质异能态俘获截面的研究

合理地给出了复合核反应光子穿透系数及同质异能态俘获截面的计算公式,其中包括统计和非统计过程.通过求解级联γ退激过程计算光子穿透系数,既合理地扣除(n,γn)过程,又包括首次γ跃迁至中子分离能B_n以上能级的贡献.以4MeV以下中子和⁵⁹Co及¹⁰³Rh的反应为例,比较用不同方法计算的光子穿透系数,计算同质异能态俘获截面并和实验数据进行比较,最后对结果进行了分析和讨论.     

恒星能量下核子俘获反应率的晕核效应

恒星能量下俘获截面很难直接测量。¹⁰Be（n，γ）¹¹Be俘获反应涉及到非均匀宇宙大爆炸核合成，无直接测量实验截面数据。利用转移反应¹⁰Be（d，p）¹¹Be的渐近归一化系数（ANC）方法，计算了¹⁰Be（n，γ）¹¹Be俘获反应截面和反应率。¹¹Be是中子晕核。研究表明，在恒星能量下俘获到晕态的截面和反应率显著增大。     

描述中子辐射俘获截面非统计效应的统一表象

基于对俘获态及终态波函数的自洽描述,建立了计算核子辐射俘获反应非统计效应的统一表象.应用这一模型对²⁷Al、⁵⁵Mn、⁸⁹Y和²⁰⁸Pb等四个核素在中子能量为0。1—20MeV能区计算了中子辐射俘获截面,并与实验值进行了比较.     

12C快中子辐射俘获反应中的共振现象

主要研究中子辐射俘获反应中的共振现象,利用DSD模型计算激发能量在5—25MeV能区的¹²C(n,γ0)反应截面与E_n=9MeV时的角分布.所考虑的反应机制包括复合核俘获、直接和半直接俘获、复弹性和非弹性散射道的辐射俘获.计算表明,矮共振的峰值在激发能量为13MeV处;巨共振的峰值位置在激发能量21MeV处.计算结果与实验符合较好.     

中重核中子辐射俘获γ射线强度函数研究

假设退激过程中除包含巨偶极共振模式外还存在⁶He,⁶Li,⁶Be,⁷Li和⁷Be等粒子集团激发态的退激过程.本文对这一物理假定作了进一步分析.利用据此建立的包括这些过程在内的γ射线强度函数,计算了在核素⁹³Nb,¹⁸¹Ta和天然元素Ag上入射中子能量在0.01—5MeV能区以及在核素¹⁹⁷Au上入射中子能量在0.01—10MeV能区的中子辐射俘获反应截面和γ能谱,得到了与实验数据较好符合的结果.特别是可以较好地解释γ能谱中5.5MeV之后的反常突起.这表明,上述物理假定适用于中重核中子辐射俘获反应.     

直接俘获截面中的核晕效应

恒星能量下俘获截面非常难于直接测量.因此,通常借助于非直接方法或从最低能量下的实验数据外推到天体物理感兴趣能区.首先证明了用渐近归一化常数方法得到的结果近似与模型无关.因此,转移反应的渐近归一化常数方法处理提供了一可靠的途径用以确定恒星能量下的俘获截面. 鉴于此优点, 用渐近归一化常数方法计算了¹⁰Be(n,γ)¹¹Be反应的俘获截面. ¹¹Be是一个众所周知的具有两弱束缚态的晕核.作为一个典型的例子,演示了俘获到晕态的辐射俘获截面明显增大, 证明了入射中子波函数与晕的伸展尾部有较大重叠是俘获截面异常增大的原因.     

铕的快中子俘获截面

使用大液体闪烁探测器,相对于金的俘获截面测量了铕(Eu)六个能量点的中子俘获截面值;用光学模型和统计理论计算了¹⁵¹Eu和¹⁵³Eu在0.1—2.0MeV能区的中子俘获截面;对实验测量和理论计算结果进行了分析和讨论.     

关于"太阳在银河系中所受引力与到银心距离r的关系"的讨论

讨论了银道面内的引力场强分布和太阳在银河系中所受引力与到银心距离r的关系，指出引力场强g并不是与r的平方成反比，这是由于银河系的大小和形状不能忽略造成的．强调了万有引力定律的适用条件．     

On the calculation of the bremsstrahlung in the region of the plasma frequency

On the basis of the classical theory of radiation produced in incomplete Coulomb interaction, a formula is derived for the coefficient of the bremsstrahlung of fully ionized plasma. In the region of rectilinear approximation a comparison is made with the results of the quantum formula derived from the Born approximation. Furthermore, the influence of dispersion upon the emission coefficient is taken into account; some relations for the region of dispersion are given.     

Dependence of the Intensity of the Spectral Lines and the Composition of the Sample and the Plasma Parameters of the Unipolar Arc

The investigation was made of the dependence of the intensity of Tl, Ga, Mo, Mg, Mn, Sn, Bi, Ni, Zn, Pt and Au spectral lines and the plasma parameters (temperature T, electron concentration n_e, degree of 6 ionnization α) from concentration of lithium additive.     

On the predictability of the positions of the convergence zones in the ocean

The disagreement between the experimental and calculated positions of the first convergence zone are known from many publications. The most probable cause for such a disagreement, namely, the incorrect specification of the input data for the calculations, is considered. The lack of simultaneity between the hydrological surveys of the region and the acoustic experiments is emphasized. The experimental data obtained by the author in five ocean regions are presented. These data characterize the diurnal variability of the distance from the source to the nearest boundary of the convergence zone. The relations proposed by different researchers for calculating the sound speed from the temperature, salinity, and hydrostatic pressure are analyzed. It is shown that these relations lead to a substantial difference in the estimated depth dependence of the hydrostatic gradient of the sound speed. The position of the first convergence zone is calculated for the propagation conditions determined by vertical temperature and salinity profiles with the subsequent recalculation of these profiles into sound speed profiles by using eight different formulas known from the literature. It is shown that different formulas lead to different values of the distance to the first zone; this difference is substantially greater than that between the calculations and experiment. The necessity of improving the recalculation relations in view of the experimental data on sound propagation in natural oceanic waveguides, including the data on the actual positions of the convergence zones, is emphasized.     

Extracting the wavefunction of the LSP at the LHC

We consider associated production of squarks and gluinos with the lightest supersymmetric particle (LSP), or states nearly degenerate in mass with it. Though sub-dominant to pair production of color SU(3)-charged superpartners, these processes are directly sensitive to the wavefunction composition of the lightest neutralinos. Exploiting event-shape variables - including some introduced here for the first time - we are able to identify the composition of the LSP by selecting events involving a single high-pT jet recoiling against missing transverse energy. We illustrate the proposed technique on a set of benchmark cases and propose methods for applying these results in more realistic experimental environments.     

Set the controls for the heart of the Sun

In this paper we describe experiments conducted with high-power lasers that are attempting to replicate, for a very short time and in miniature, conditions found in the Sun. Experiments to date have reached conditions in the outer part of the Sun. To reach the Sun's centre requires compression of material to very much greater than solid density and heating to over ten million degrees. To achieve this, a new class of experiments and a new generation of high-power lasers are required.     

On the Question of the Source of the Apokamp

Technical Physics - The object of this work is the apokamp—a new type of plasma jet, which is formed from a bright offshoot emerging at the bending point of a channel of a high-voltage...