Type Ia Supernova Cosmology

The primary agent for Type Ia supernova cosmology is the uniformity of their appearance. We present the current status, achievements and uncertainties. The Hubble constant and the expansion history of the universe are key measurements provided by Type Ia supernovae. They were also instrumental in showing time dilation, which is a direct observational signature of expansion. Connections to explosion physics are made in the context of potential improvements of the quality of Type Ia supernovae as distance indicators. The coming years will see large efforts to use Type Ia supernovae to characterise dark energy.     

Supernovae and the origin of the solar system

This review concentrates on recent ideas involving a relationship between the early solar system and supernova explosions. It summarizes briefly the data that has helped inspire those ideas. Because the true relationship is still unknown and generates controversy, the distinct ideas are introduced singly in the historical context of their origins, and the active sense of surprise and controversy is visible. Quotations from pivotal papers are used as part of the exposition. The subject involves equally the isotopic anomalies detected in meteorites and the dynamic events of galactic evolution, nucleosynthesis, and protosolar collapse. Whatever the correct situation is, new connections have been found between the origin of the elements and the formation of the solar system. The objective of this review is to enable interested space scientists to quickly identify the competing points of view and the experiments and theories that have led to them.     

Dust in Supernovae and Supernova Remnants I: Formation Scenarios

Supernovae are considered as prime sources of dust in space. Observations of local supernovae over the past couple of decades have detected the presence of dust in supernova ejecta. The reddening of the high redshift quasars also indicate the presence of large masses of dust in early galaxies. Considering the top heavy IMF in the early galaxies, supernovae are assumed to be the major contributor to these large amounts of dust. However, the composition and morphology of dust grains formed in a supernova ejecta is yet to be understood with clarity. Moreover, the dust masses inferred from observations in mid-infrared and submillimeter wavelength regimes differ by two orders of magnitude or more. Therefore, the mechanism responsible for the synthesis of molecules and dust in such environments plays a crucial role in studying the evolution of cosmic dust in galaxies. This review summarises our current knowledge of dust formation in supernova ejecta and tries to quantify the role of supernovae as dust producers in a galaxy.     

Dust in Supernovae and Supernova Remnants II: Processing and Survival

Observations have recently shown that supernovae are efficient dust factories, as predicted for a long time by theoretical models. The rapid evolution of their stellar progenitors combined with their efficiency in precipitating refractory elements from the gas phase into dust grains make supernovae the major potential suppliers of dust in the early Universe, where more conventional sources like Asymptotic Giant Branch (AGB) stars did not have time to evolve. However, dust yields inferred from observations of young supernovae or derived from models do not reflect the net amount of supernova-condensed dust able to be expelled from the remnants and reach the interstellar medium. The cavity where the dust is formed and initially resides is crossed by the high velocity reverse shock which is generated by the pressure of the circumstellar material shocked by the expanding supernova blast wave. Depending on grain composition and initial size, processing by the reverse shock may lead to substantial dust erosion and even complete destruction. The goal of this review is to present the state of the art about processing and survival of dust inside supernova remnants, in terms of theoretical modelling and comparison to observations.     

Equivalent Electric Circuit Models of Coronal Magnetic Loops and Related Oscillatory Phenomena on the Sun

Coronal loops, which trace closed magnetic field lines, are the primary structural elements of the solar atmosphere. Complex dynamics of solar coronal magnetic loops, together with action of possible subphotospheric dynamo mechanisms, turn the majority of the coronal loops into current-carrying structures. In that connection none of the loops can be considered as isolated from the surroundings. The current-carrying loops moving relative to each other interact via the magnetic field and currents. One of the ways to take into account this interaction consists in application of the equivalent electric circuit models of coronal loops. According to these models, each loop is considered as an equivalent electric LCR-circuit with variable inductive coefficients L, capacitance C, and resistance R, which depend on shape, scale, position of the loop with respect to neighbouring loops, as well as on the plasma parameters in the magnetic tube. Such an approach enables to describe the process of electric current dynamics in the groups of coronal loops, as well as the related dynamical, energy release and radiation processes. In the present paper we describe the major principles of LCR-circuit models of coronal magnetic loops, and show their application for interpretation of the observed oscillatory phenomena in the loops and in the related radiation.     

Chebyshev超谱粘性法在推进剂供应管路非定常流动分析中的应用

基于一维管道瞬变流理论和数值谱方法,给出了求解推进剂供应系统管路内液体非定常流动控制方程的Chebyshev超谱粘性法。与常规谱方法相比,该方法有效地克服了由于解的间断或大梯度变化而发生的非物理振荡现象,而且在一定程度上加快了收敛速度,提高了计算效率。以一段两端分别连接贮箱和阀门的等截面圆直管为例,利用该方法对阀门关闭后管道内水击现象进行了计算,给出了相应的水击压力仿真结果,并分别与采用特征线方法和传统谱方法求得的结果进行了对比分析,验证了方法的正确性和优越性。     

Grain Surface Models and Data for Astrochemistry

The cross-disciplinary field of astrochemistry exists to understand the formation, destruction, and survival of molecules in astrophysical environments. Molecules in space are synthesized via a large variety of gas-phase reactions, and reactions on dust-grain surfaces, where the surface acts as a catalyst. A broad consensus has been reached in the astrochemistry community on how to suitably treat gas-phase processes in models, and also on how to present the necessary reaction data in databases; however, no such consensus has yet been reached for grain-surface processes. A team of \({\sim}25\) experts covering observational, laboratory and theoretical (astro)chemistry met in summer of 2014 at the Lorentz Center in Leiden with the aim to provide solutions for this problem and to review the current state-of-the-art of grain surface models, both in terms of technical implementation into models as well as the most up-to-date information available from experiments and chemical computations. This review builds on the results of this workshop and gives an outlook for future directions.     

Markets and Models for Large-Scale Courseware Development

Computer-aided instruction (CAI) has not achieved widespread use, even though experimental results have been promising, because of a complex of technical, economic, and social factors. The problems these factors produce might be overcome if a major ?market success? could be achieved with CAI systems. One potentially high-volume market, having probably a lower resistance to profound innovation than other sectors of education, is the junior college. To achieve a market success which would catalyze public and private investment to sustain the growth and dissemination of CAI requires technical solutions in the areas of hardware, software, and courseware. Courseware is a term designating the applications programs for CAI systems and associated textual, audio-visual, and other materials of instruction. Two different approaches to the production of courseware and their underlying philosophies are discussed and contrasted. The extent to which these different models of courseware design and development might lead toward the goal of mass dissemination is highlighted.     

P. Ruiz-Lapuente,R.; Canal,J.; and Isern (eds.). Thermonuclear Supernovae

Space Science Reviews -     

飞船自主应急返回控制参数确定方法及应用

当飞船在无地面测控支持的运行段飞行时,必须考虑故障情况下飞船自主返回应急着陆区的控制参数确定问题。本文根据飞船自主应急返回的主要特点和应急着陆区的选取原则,在分析飞船再入动力学过程和实际测量数据的基础上,确立了一种飞船自主应急返回的控制参数计算方法及流程,并简要介绍了该方法在“神舟4号”等飞船测控任务中的应用。     

Atmospheric Attenuation Models for Satellite-To-Earth Links

In an earlier paper by the authors1 it was mentioned that atmospheric attenuation effects could be included by assuming that the attenuation is directly proportional to number of air masses. While this assumption is valid for the optical region, it is not true in the microwave region (1 to 40 GHz). For a clear atmosphere, the two constituents which absorb microwaves are oxygen and water vapor. An analysis of the atmospheric attenuation data for the microwave region has been made and some rather simple expressions for computing the attenuation as a function of zenith angle are developed with an accuracy suitable for satellite antenna footprint calculations.     

收益管理系统中的几个关键模型

介绍了国内首例自主开发的收益管理系统中的部分运算模型，给出了需求预测、超售、座位优化控制中的一些核心算法。提出了基于C-均值聚类的航班预测模型、基于二项分布的超售计算模型、基于EMSR的多航段座位优化模型、基于期望边际收益的团体置换价模型等．并介绍了上述模型的运行效果。     

雷达舰船目标回波建模研究

阐述了根据电磁波几何绕射理论所建立的舰船目标雷达回波模型,利用该模型可产生多种假设目标的回波数据,用于弥补科研试验过程中所需的多种条件下的雷达目标回波数据,所建模型在实际试验中得到了较好的应用.     

Overall Detection Probability for Fluctuating and Nonfluctuating Target Models

The power selection of a search radar is best obtained in the framework of the overall detection probability concept. This concept is here applied to fluctuating target models for single- and multiple-scan detection. The approach combines the pulse train statistics over the detection interval to the mean target statistics over the search region and directly relates the overall detection probability POD to a single system parameter ?0, proportional to the transmitted power.     

Dynamo Models for Planets Other Than Earth

Observations from planetary spacecraft missions have demonstrated a spectrum of dynamo behaviour in planets. From currently active dynamos, to remanent crustal fields from past dynamo action, to no observed magnetization, the planets and moons in our solar system offer magnetic clues to their interior structure and evolution. Here we review numerical dynamo simulations for planets other than Earth. For the terrestrial planets and satellites, we discuss specific magnetic field oddities that dynamo models attempt to explain. For the giant planets, we discuss both non-magnetic and magnetic convection models and their ability to reproduce observations of surface zonal flows and magnetic field morphology. Future improvements to numerical models and new missions to collect planetary magnetic data will continue to improve our understanding of the magnetic field generation process inside planets.     

碳基及陶瓷基复合材料CVI工艺数值模拟的相关数学模型

概述阐述了ＣＶＩ数值模拟的基本原理及几种相关的数学模型,提出了２Ｄ碳／碳复合材料的几隙结构模型,并验证了该模型的可行性。     

塞式喷管推力模型的建立与实验验证

 为了能够方便快捷地对塞式喷管发动机的性能做出准确的预示,通过理论分析,结合塞式喷管的流场特征,提出了一种塞式喷管壁面压强分布的数学模型。在此基础上,分别建立了全长型和截短型的塞式喷管的推力模型。通过与实验的对比分析,模型与实验数据基本吻合,验证了塞式壁面压力分布的数学模型以及在此基础上建立的推力模型,可以作为塞式喷管发动机性能预示的有效工具。