中介时序逻辑系统MTL的模型论性质

时序逻辑作为一种把时间概念直接引入其形式系统的逻辑系统,它具有较强的表达能力,近年来在计算机科学领域获得了广泛的应用.基于中介逻辑对时序逻辑进行多值扩充,建立了一种中介时序逻辑系统MTL(Medium Temporal Logic).讨论了它的形式系统和语义解释,但未论及其完备性.本文对MTL系统作进一步的讨论.在一可传结构下,讨论了它的可传、连通和过滤等模型论性质,为进一步讨论MTL系统的完备性作了理论上的准备.     

基于中介逻辑的多模态逻辑系统

多模态逻辑作为模态逻辑的扩充，是模态逻辑进行时态和动态扩充的基础。中介逻辑是一个新的逻辑系统，自创立后得到了很大发展，并在数理逻辑及计算机科学领域中得到广泛应用。为将中介逻辑进行时态和动态扩充，本文构造了一种基于中介逻辑的多模态逻辑系统ＭＭＫ，讨论了它的推理规则和语义解释，并证明了ＭＭＫ的可靠性和完备性，在此基础上给出了一种基于中介逻辑的时态逻辑系统ＭＴ，对它的可靠性和完备性进行了讨论。最后，分析了相应的经典多模态逻辑系统与ＭＭＫ系统及经典时态逻辑系统和ＭＴ系统之间的关系。     

中介公理集合论系统与经典公理集合论系统的关系——形式证明部分

在中介公理集合论系统（ＭＳ）中重新定义了良集的概念，讨论了它的性质。证明良集完全满足经典公理集合论系统（ＺＦＣ－：ＺＦＣ系统中去掉正则公理）的全部公理，且其配套的逻辑系统恰为中介逻辑的二值子系统ＦＩ＊ＭＬ，说明整个经典数学也能奠基于ＭＳ之上，从而最终回答了中介数学与经典数学的包含关系问题。     

基于中介理论与交通特性的终端区态势评价

终端区交通态势的准确度量是制定并实施流量管理措施的重要依据之一。通过提取终端区宏观与微观的交通特性,从进离场及总量3个维度构建态势的指标描述,并进一步采用中介理论中的真值程度度量与熵权法建立了一种客观的终端区飞行区交通态势模糊综合评价方法,实现客观、准确的交通态势判别与样本间量化比较。选取国内典型繁忙终端区的实测数据,验证了评价方法与特性指标的有效性。     

基于多孔介质模型的指尖密封泄漏流动分析

将指尖密封处理为多孔介质,把压力梯度作为多孔介质动量方程中的源项,根据试验结果确定了源项中的系数,结合指尖密封的结构参数提出了用于指尖密封泄漏的多孔介质模型,利用该模型计算结果与试验结果吻合较好,证明利用该模型模拟指尖密封泄漏是可行的.流场计算结果表明:指尖密封与转子接触部分的孔隙率对泄漏影响比较大,指尖密封的承压部分主要为后挡板内径以下区域.      

多孔介质隔热材料中的辐射热传递分析

新型的多孔材料以其重量轻、强度高备受航天工程设计人员的亲睐,尤其是作为隔热材料使用,可以说是航天工程热防护系统的热门材料.多孔介质在辐射热传递方面具有吸收发射和散射的功能,这些功能在其接受外来热流的作用下,于内部达到热能量平衡,求解这一平衡方程就可以求出辐射热流在材料中的分布.由于求解这一方程的困难,许多学者对材料特性...     

相变光盘多层膜系结构的最佳光匹配研究

论述了相变光盘最佳膜系结构的设计。采用导纳矩阵法计算膜系的能量反射率，用量优化计算方法编程计算，提出了第二大极值解作为在工艺上可行的实用光盘的膜系结构，并按这种膜系结构制作样品，其擦写循环数达１００万次上。     

Halo White Dwarfs and Baryonic Dark Matter

We describe the formation of hot intergalactic gas along with baryonic remnants in galaxy halos. In this scenario, the mass and metallicity of the hot intracluster and intragroup gas relates directly to the production of baryonic remnants during the collapse of galactic halos. We construct a schematic but self-consistent model in which early bursts of star formation lead to a large remnant population in the halo, and to the outflow of stellar ejecta into the halo and ultimately the Local Group. We consider local as well as high redshift constraints on this scenario. This study suggests that the microlensing objects in the Galactic halo may predominantly be 0.5M white dwarfs, assuming that the initial mass function for early star formation favored the formation of intermediate mass stars with m 1M. However, the bulk of the baryonic dark matter in this scenario is associated with the ejecta of the white dwarf progenitors, and resides in the hot intergalactic medium.     

MP＊中的等值完全析取范式

讨论中介逻辑命题演算扩张系统ＭＰ＊中在等值意义下的完全析取范式的存在性和唯一性。引入ＭＰ＊中等值全板范式的概念，并用分步构造法证明这种范式在等值意义下是存在的，且是唯一的。     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.