超新星的前身星阶段fp壳层的电子俘获

基于核的壳层模型，本文讨论了大质量恒星的超新星前身星阶段核的fp壳层电子俘获，分析中引入了一高斯函数来表征Gamow-Teller跃迁强度分布，结果表明，由于这一修正，在高密度下，电子俘获率较前人给出的结果有较大幅度的增加。     

丰中子氮同位素β-衰变的理论研究

使用壳模型系统地研究了丰中子氮同位素的β^-衰变,并对其衰变子核^18,19,20,21O的能级结构性质给出理论计算,所得结果与实验符合较好.研究了^18,19,20N核的Gamow-Teller允许型β^-衰变的特性,对与近期实验观测不一致之处进行了讨论和分析.预言了²¹N的β^-衰变及其子核高激发态的能级结构性质.这些计算将对氮同位素的实验研究很有帮助. 关键词： 中子滴线 -衰变')" href="#">β^-衰变 氮同位素 壳模型     

超新星爆发环境核素56,57,59,60Co的电子俘获

基于壳模型与Random Phase Approximation理论, 利用Shell-Model Monte Carlo方法, 研究了超新星爆发环境核素^56,57,59,60Co的电子俘获与电子丰度变化率. 我们的结果与利用Aufderheide方法计算的结果进行了误差对比. 结果表明: 电子俘获率受温度和密度的影响大大增加, 甚至增加达6个数量级以上(如在ρ₇=0.43, Y_e=0.48核素^57,59,60Co). 另一方面, 随着温度和密度的增大, 电子丰度变化率大大降低, 甚至减小达5个数量级以上(如在ρ₇=5.86, Y_e=0.47核素⁵⁹Co). 通过对误差因子的分析表明, 在低温低密度环境二种结果误差较大; 而在高温高密度环境, 二种结果误差相对较小. 关键词： 电子俘获 超新星     

μ~-介子在Be~7原子核上的俘获

利用考虑到重正化效果的普适V-A理论,本文计算了μ_-被Be~7俘获后跃迁到Li~7的基态与第一激发态的俘获几率,Li~7核第一激发态的极化,以及由此跃迁到其基态时放出γ光的偏振度,其中对于不同的超精细结构态分别进行了计算,计算过程中,采用了壳层模型的原子核波函数。并假定忽略二次效应下,S态的四个核子没有参加作用。     

基于投影壳模型的β衰变理论

在投影壳模型(PSM)理论框架下, 发展了计算Gamow-Teller(GT)跃迁的新方法. PSM波函数由若干变形多准粒子组态投影基的线性组合表达. 由该波函数可以计算GT算符(σ_μτ_±)的跃迁矩阵元. 研究表明, 计算的第一个例子可以再现log ft或B(GT)实验值, 同时预言了母核的某些低激发态的GT跃迁比基态的强, 此效应在恒星温度下, 会增强原子核的衰变率.     

低能He2+-He反应中单电子俘获微分散射过程的实验研究

利用冷靶反冲离子动量谱仪装置系统研究了20—40 keV He²⁺-He碰撞体系的态选择单电子俘获过程,实验获得了单电子俘获过程的态选择截面以及角微分截面.在所研究的能区范围,电子俘获到L壳层的截面最大,为主要的反应道,这与分子库仑过垒模型的反应窗理论的预测一致.实验测量的态选择截面与原子轨道紧耦合的计算结果很好地符合,与光谱方法的测量结果存在一定的差别,主要原因是光谱方法不能测量完整的反应通道信息.实验结果表明,总角微分截面在小角度范围主要来源于电子俘获到基态的贡献,在大角度范围主要来自电子俘获到激发态的贡献;电子俘获到基态的和激发态的角微分截面均出现振荡结构,这种振荡来源于电子俘获反应中分子轨道之间的相干效应.实验测量的角微分截面与其他实验和紧耦合方法的计算结果进行了比较和分析. 关键词： 冷靶反冲离子动量谱仪 态选择电子俘获 态选择截面 角微分截面     

对氯苯腈的双色共振双光子电离和质量分辨阈值电离光谱

本文利用双色共振双光子电离和质量分辨阈值电离光谱技术,研究了对氯苯腈分子第一电子激发态S₁和离子基态D₀的振动特征,确定了对氯苯腈分子S₁←S₀电子跃迁的激发能为35818±2 cm^–1,精确的绝热电离能为76846±5 cm^–1.对氯苯腈分子³⁵Cl和³⁷Cl两种同位素有相同的激发能和电离能以及相似的振动特征.采用高精度密度泛函方法,计算了对氯苯腈分子在中性基态S₀、第一电子激发态S₁、离子基态D₀的结构参数和振动频率,分析了电子激发和电离过程中对氯苯腈分子结构和振动频率的变化,并对激发态和离子基态的振动光谱进行了归属,振动光谱上的活性振动大多数是苯环平面内的弯曲振动.通过比较对氯苯酚、对氯苯胺、对氯苯甲醚、对氯苯腈与苯酚、苯胺、苯甲醚、苯腈分子的跃迁能,分析了取代基Cl原子与苯环之间的相互作用及其对分子跃迁能的影响.     

电荷屏蔽对Ⅱ型超新星瞬时爆发能量的影响

讨论了电荷屏蔽效应对WS15M_⊙前身星模型瞬时爆发能量的影响,对电子俘获率的计算基于平均重核模型,数值模拟表明电荷屏蔽降低了电子俘获率,延长了爆发时间,使中微子泄漏的总能量增加,从而导致激波的能量略微降低.给出的方法可以适用于其他考虑电荷屏蔽效应的超新星数值模拟. 关键词： 超新星 瞬时爆发 数值模拟 电荷屏蔽     

μ-介子在Be7原子核上的俘获

利用考虑到重正化效果的普适V-A理论,本文计算了μ^-被Be⁷俘获后跃迁到Li⁷的基态与第一激发态的俘获几率,Li⁷核第一激发态的极化,以及由此跃迁到其基态时放出γ光的偏振度,其中对于不同的超精细结构态分别进行了计算,计算过程中,采用了壳层模型的原子核波函数。并假定忽略二次效应下,S态的四个核子没有参加作用。     

半导体量子点中极化子的跃迁能量

研究了半导体量子点中极化子的激发态性质。采用Huybrechts线性组合算符和幺正变换方法,计算了量子点中极化子的振动频率、基态能量、第一激发态能量、由第一激发态向基态的跃迁能量和跃迁频率。分别讨论了电子-LO声子在强弱两种耦合情况下极化子的跃迁能量和跃迁频率。数值计算结果表明,跃迁能量ΔE和跃迁频率ω均随量子点有效受限长度l₀的增加而减少,且随电子-声子耦合强度α的增加而减少。     

Carmeli's Cosmology Fits Data for an Accelerating and Decelerating Universe Without Dark Matter or Dark Energy

A new relation for the density parameter Ω is derived as a function of expansion velocity υ based on Carmeli's cosmology. This density function is used in the luminosity distance relation D _L. A heretofore neglected source luminosity correction factor (1 − (υ/c)²)^−1/2 is now included in D _L. These relations are used to fit type Ia supernovae (SNe Ia) data, giving consistent, well-behaved fits over a broad range of redshift 0.1 < z < 2. The best fit to the data for the local density parameter is Ω_m = 0.0401 ± 0.0199. Because Ω_m is within the baryonic budget there is no need for any dark matter to account for the SNe Ia redshift luminosity data. From this local density it is determined that the redshift where the universe expansion transitions from deceleration to acceleration is z _t = 1.095^+0.264 _−0.155. Because the fitted data covers the range of the predicted transition redshift z _t, there is no need for any dark energy to account for the expansion rate transition. We conclude that the expansion is now accelerating and that the transition from a closed to an open universe occurred about 8.54 Gyr ago.     

超新星研究进展

本文先介绍超新星巡天和分类,简要地论述历史超新星SN 1006一千年,接着讨论核心塌缩超新星物理和具体事例（SN1987A 20年、 SN2006gy、 2008D）及超新星与γ射线暴的联系,文章重点讨论SNIa 和宇宙学,评述了SNIa在宇宙学中的应用和哈勃常数的确定,最后指出超新星研究目前存在的问题。     

Constraints from Type Ia supernovae on the Λ-CDM model in Randers-Finsler space

Gravitational field equations in Randers-Finsler space of approximate Berwald type are investigated. A modified Friedmann equation and a new luminosity distance-redshift relation is proposed. A best-fit to the Type Ia supernovae (SNe) observations yields that the Ω_Λ in the Λ-CDM model is suppressed to almost zero. This fact indicates that the astronomical observations on the Type Ia SNe can be described well without invoking any form of dark energy. The best-fit age of the universe is given. It is in agreement with the age of our galaxy.     

A Model of Light from Ancient Blue Emissions

A model is presented to explain the luminar distances and associated red-shifts from ancient supernovae. Light frequencies of supernovae type Ia (SNe Ia) vary smoothly with time, decreasing from singularity to present and intergalactic luminar distances are described as linear combinations of Hubble expansion and smaller components from the time-dependent decrease of emission frequencies. When tested with current cosmic matter densities, SNe Ia distances, red-shifts and the Hubble constant the errors between this model and the vacuum energy model favor this new model, though our model suffers from mathematics about zero. An expression between energy and frequency, derived from the model, reducing to the Planck equation for short observation intervals is also discovered and estimated to within 10% using current SNe Ia data. We also propose a relationship for the deceleration of frequency over time, solve at infinity and discover frequency and time will eventually become uncoupled.     

Properties of SN Ia progenitors from light curves and spectra

With recent advances in theory and observations, direct connections emerge between the progenitors of Type Ia Supernovae (SNe Ia) and the observed light curves and spectra. A direct link is important for our understanding of the supernovae physics, the diversity of SNe Ia and the use of SNe Ia for high-precision cosmology because the details of the explosion depends sensitively on the initial conditions and the explosion scenario(s) realized in nature. Do SNe Ia originate from SD- or DD systems, and do they lead to M_Ch mass explosions or dynamical mergers? Does the statistical distribtion of SNe Ia depend on their environment which can be expected to change with redshift? In this contribution, we will exam from the theoretical point of view the tell-tails for this connection, their consistency with the observations, and future directions. In a first section, we present the physics of the explosion, light curves and spectral formation in a nutshell to help understanding the connection. For details of the progenitor evolution and explosion physics, we refer to reviews and the other contributions in this issue. Each of the topical sections starts with a brief general review followed by a more detailed discussion of specific results. Because the youth of the field, some bias is unavoidable towards results obtained within our collaborations (and FSU). The imprint of the metallicity, progenitor stars and properties such as the central density of the exploding WD are presented. IR spectroscopy, polarimetry and imaging of SNR remnants are discussed as a tool to test for the WD properties, magnetic fields and asymmetries. We discuss different classes of Type Ia supernovae, and their environment. Possible correlations between the spectroscopic and light curve properties of SN Ia are discussed. Finally, the overall emerging picture and future developments are discussed.     

Birthrates and delay times of Type Ia supernovae

Type Ia supernovae (SNe Ia) play an important role in diverse areas of astrophysics, from the chemical evolution of galaxies to observational cosmology. However, the nature of the progenitors of SNe Ia is still unclear. In this paper, according to a detailed binary population synthesis study, we obtained SN Ia birthrates and delay times from different progenitor models, and compared them with observations. We find that the Galactic SN Ia birthrate from the double-degenerate (DD) model is close to those infe...     

Effect of lattice relaxation on spin density of nitrogen-vacancy centers in diamond and oscillator strength calculations

Using a generalized Hubbard Hamiltonian, many-electron wavefunctions of negatively charged (NV⁻) and neutral nitrogen-vacancy (NV⁰) centers in diamond were calculated. We report the effect of symmetric relaxation of surrounding atoms on the spin density, calculated from the many electron wavefunctions in the ground and excited states. We evaluated the error, that, arises in estimation of spin density when lattice relaxation effect is neglected in Electron Paramagnetic Resonance experiment and showed that the ground state spin density distribution is accessible in outward relaxations. The computed oscillator strengths give a higher efficiency for the 1.945 eV photoluminescence (PL) line of NV⁻ with respect to 2.156 eV PL line of NV⁰ which agrees well with experiment. This result is explained based on the largest the ground state spin among available values for the NV⁻ with respect to NV⁰. The transition probability between degenerate ground and excited states slightly depends on the S _z value. Finally, we report on the electronic configurations which contribute to the ground and excited states and discuss the population variation of electronic configurations with relaxation.     

The low-lying level structure of87Rb

The low-lying states of⁸⁷Rb are studied in the framework of a quasiparticle-core coupling model. The agreement between the calculated and experimental level spectra, stripping strength, ground state static electromagnetic moments and theE2 transition rate of the first excited state is good. Electromagnetic moments and transition rates for other excited states are predicted.     

Synchrotron radiation from relativistic electrons in intense magnetic fields

The synchrotron radiation spectrum is calculated for relativistic electrons in the case where no restriction is placed on the strength of the magnetic field. It is shown that in intense fields H? H₀ = m²c³/e₀? =4.41 · 10¹³ G a major contribution to the total radiation intensity comes from transitions to the ground state and also to weakly excited levels. In particular, the contribution from transitions to the ground state (final electron energy E' =mc²) for electrons of initial energy E = 10 MeV in a field H = 2H₀ is 14% of the contribution from transitions to highly excited states (E'?mc²).     

Spectroscopy of9He with the (13C,13O)-reaction on9Be

First results of the double-charge-exchange reaction⁹Be(¹³C,¹³O)⁹He, E_Lab=380 MeV, are presented. The ground state and an excited state at 3.8 MeV are clearly seen. A preliminary value of the⁹He mass excess is obtained: 41.5±0.6 MeV. Spectra of of the⁹Be(¹³C,¹⁴O) He-reaction have been measured with high resolution. The ground state transition appears as a pronounced sharp peak, but no other narrow peaks are observed.