压缩氘氚球的热核燃烧特性研究

本文利用LARED-S程序模拟了等密度和等压力条件下压缩氘氚球的热核反应燃烧过程.对于等密度模型,模拟了两个具体算例,与国外计算结果进行了比较,验证了程序的可靠性.对于等压力模型,利用数值模拟给出了热核反应燃烧与压缩氘氚球初始状态之间的关系曲线,分析发现,氘氚装量、压力和主燃料密度的增加有利于提高热核反应放能和燃耗,中心热斑的温度和面密度分别达到70—80 MK和3—4 kg·m^-2时热核反应才有显著的放能,提高主燃料密度,可以适当放宽对中心热斑的点火要求.最后对实际点火靶进行了数值模拟并且与等压力模拟计算结果进行了比较分析.     

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.     

α粒子的慢化过程对D-T等离子体聚变燃烧的影响

在双温聚变燃烧点模型框架下，对比D-T等离子体聚变燃烧过程中α粒子能量逐步沉积与瞬时沉积两种描述的等离子体温度、离子数密度随时间的变化，在不同的密度条件下作了计算，考察了α粒子的慢化过程对D-T聚变点火的影响.发现考虑α粒子的慢化过程后，D-T等离子体峰值温度的出现将会推迟若干皮秒甚至几十皮秒，在较低的初始温度密度条件下，时间推迟得更多些.等离子体的峰值温度比α粒子能量瞬时沉积描述也会下降13keV左右. 关键词： α粒子 聚变燃烧 能量沉积 慢化过程     

加氚对D-3He系统聚变燃烧过程的影响

对加少量氚的D-³He聚变系统的点火燃烧过程进行了数值模拟研究,得到了有关的物理图象和一些主要计算结果。研究结果表明,加少量氚可以解决D-³He聚变系统的点火问题和加速其燃烧过程,从而提高燃耗。     

Physikalische Probleme der Untersuchungen zur Kernfusion in Kondensierter Materie

An avalanche-like increase of research activities in the field was caused by the spectacular announcements and publications about the observation of nuclear fusion processes during the infusion of deuterium into metals. Though, the original claims by Fleischmann and Pons concerning the observation of macroscopic amounts of heat so far seem not to be approved in a quantitative manner by other groups, there are indications for the start of a new interesting field of research at the border between nuclear physics and solid state physics – investigations of nuclear fusion processes in condernsed matter. First conclusions drawn here about possible mechanisms of such processes have to be considered neither complete nor final.     

非Maxwell分布下平均热核反应率的计算

研究氘氚（DT）服从不同的速度分布函数时平均热核反应率的计算,当T服从Maxwell分布,D服从Maxwell分布、单能分布、一类特殊的非Maxwell分布时,用Monte Carlo方法（蒙卡方法）和直接积分两种方法同时计算DT的平均热核反应率,并验证蒙卡方法的正确性.利用蒙卡方法计算非Maxwell分布时的DT平均热核反应率,与Maxwell分布下的结果有较大的差别,说明在类似的情况下如果采用热动平衡下的平均热核反应率会引入较大的误差,相关认识可供非平衡效应研究参考.     

速度分群情况下氘氚热核反应率的模拟与分析

研究两种原子核粒子参与反应的热核聚变,假定一种原子核粒子处于热动平衡状态,对另一种原子核粒子速度分布进行分群,推导分群热核反应率以及平均热核反应率,编制相应计算程序;以氘氚热核聚变反应为例计算分群热核反应率和相应的平均热核反应率,并与直接积分结果进行对比;同时,细致研究平均热核反应率与速度分群数目的关系.     

Differential and integral conservation laws for a relativistic compact beam torus

For a compact charged medium interacting with an intrinsic electromagnetic field, the local and integral conservation laws along trajectories are investigated. Properties of a stationary compact beam torus are discussed. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 12, pp. 56–59, December, 2008.