太阳爆发过程中的大尺度磁重联电流片:理论和观测

从理论和观测两个方面来介绍和讨论出现在太阳爆发过程中的磁重联电流片及其物理本质和动力学特征。首先介绍在理论研究和理论模型中,磁重联电流片是如何在爆发磁结构当中形成并发展的,对观测研究有什么指导意义。然后介绍观测工作是从哪几个方面对理论模型预测的电流片进行证认和研究的。第三,将介绍观测研究给出了哪些过去所没有能够预期的结果,这些结果对深入研究耀斑一CME电流片以及其中的磁重联过程的理论工作有什么重要的、挑战性的意义。第四,讨论最新的与此有关的理论研究和数值实验。最后,对未来的研究方向和重要课题进行综述和展望。     

复波场的实部和虚部对同时源波形反演的影响

高精度的成像需要准确的速度场信息,波形反演被认为是目前具有最高分辨率的速度反演方法之一.计算效率是目前全波形反演需要考虑的一个主要问题.为了很好地解决计算效率的问题,本文引入了一种高效的无串扰同时源反演方法,并详细介绍了其原理与计算流程.同时,基于此多震源同时反演方法,本文拓展出实波场反演、虚波场反演及复波场反演的三种反演策略,进而分析复波场的实部和虚部对全波形反演的影响.实验表明,相比于复波场全波形反演,无论是实波场反演还是虚波场反演,反演分辨率有所降低;相比于实波场反演,虚波场反演对初始模型的依赖性较小,目标函数的非线性较弱;最后,通过使用组合反演策略,即初始阶段采用虚波场反演,中后期阶段采用复波场反演,不仅可以降低反演的非线性,而且能够保证高精度建模.     

红巨星∈Ophiuchi的类太阳振动

最近在红巨星∈ Ophiuchi(G9.5Ⅲ)中观测到了类太阳振动.大频率间隔为4.8μHz,并证实了∈ Ophiuchi中存在非径向振动模.依据∈ Ophiuchi红巨星观测到的振动频率数据和它在赫罗图中的位置,采用恒星演化计算与恒星振动计算相结合的方法,对∈ Ophiuchi红巨星的质量、金属丰度、年龄、半径进行了初步的限制.     

A complicated solar eruption event on 2003 October 26

We present multi-wavelength observations of a complicated solar eruption event to associate with an X1.2 flare and a Coronal Mass Ejection (CME) on 2003 October 26. The soft X-ray profile shows a possibility for occurrence of two flares with peaks around 06:20 and 07:00 UT. According to our observations, there are many evidences to show that they are corresponding to two energy releases. The first one produces type II, type III, moving type IV continua, a decimetric burst (DCIM) and strong emissions at Hα, 195 and 1600 Å; While the second energy release only produces a group of RS-III bursts, DCIM and Hα emissions. It appears that the first energy release is associated with a CME, while the second CME is quiet. Such observational difference between two energy releases is found indicating two magnetic reconnection processes occurrence with different plasma situation.     

RHESSI Observations of the Neupert Effect in Three Solar Flares

Previous observations show that in many solar flares there is a causal correlation between the hard X-ray flux and the derivative of the soft X-ray flux. This so-called Neupert effect is indicative of a strong link between the primary energy release to accelerate particles and plasma heating. It suggests a flare model in which the hard X-rays are electron – ion bremsstrahlung produced by energetic electrons as they lose their energy in the lower corona and chromosphere and the soft X-rays are thermal bremsstrahlung from the “chromospheric evaporation” plasma heated by those same electrons. Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) observes in a broad energy band and its high spectral resolution and coverage of the low-energy range allow us to separate the thermal continuum from the nonthermal component, which gives us an opportunity to investigate the Neupert effect. In this paper, we use the parameters derived from RHESSI observations to trace the primary energy release and the plasma response: The hard X-ray flux or spectral hardness is compared with the derivative of plasma thermal energy in three impulsive flares on 10 November 2002 and on 3 and 25 August 2005. High correlations show that the Neupert effect does hold for the two hard X-ray peaks of the 10 November 2002 flare, for the first peaks of the 3 August 2005 flare, and for the beginning period of the 25 August 2005 flare.     

Disaster risk evaluation using factor analysis: a case study of Chinese regions

Natural Hazards - Regional risk to natural disasters is a critical multi-criteria decision-making (MCDM) problem in the literature due to the complicated and usually conflicting evaluation index...     

海洋沉积物中氧化还原敏感元素对水体环境缺氧状况的指示作用

近年来由于人为污染水体富营养化加剧,缺氧区面积不断增大,利用沉积物中氧化还原敏感元素反演水体缺氧情况已经发展成为海洋化学领域的热点研究方向。本文详细阐述了氧化还原敏感元素的富集机制,并总结了利用沉积物中氧化还原敏感元素在不同氧化还原条件下的富集程度反映海水缺氧程度和底质氧化还原状况的一系列指标,如Re/Mo、Cd/U、Th/U、V/Sc、V/(V+Ni)值,U—Mo共变模型,δ~(98/95)Mo,多指标微/痕量元素模型以及氧化还原敏感元素-有机质共变模型等。沉积物中Re、Mo含量、Re/Mo值、自生Mo/U值、Th/U值对上层水体缺氧和氧化条件区分良好,可定量指征上层水体的缺氧情况。沉积物中Re含量近似于1 ng/g(地壳值),Mo含量1μg/g(地壳值),Re/Mo值接近0.3×10~(-3),Mo—U富集系数比为(0.1～0.3)×现代海水,Th/U值2,可指示氧化环境;Re含量在10～30 ng/g,Mo含量近似于1μg/g,Re/Mo值10×10~(-3)～30×10~(-3),Mo—U富集系数比1×现代海水,Th/U值在0～2范围内,可指示缺氧环境;Re含量30 ng/g,Mo富集达到20～40μg/g,Re/Mo值接近0.7×10~(-3)(海水中Re/Mo值),Mo—U富集系数比为(3～10)×现代海水,可指示极度缺氧的硫化环境。Mo_(EF)—U_(EF)交会对数坐标图、氧化还原敏感元素-有机质共变模型指标可定性分析上层水体的缺氧情况;V/(V+Ni)值对于次氧化沉积物指示效果不佳;Cd/U值在次缺氧条件下的变化机制复杂,还需进一步研究。生物扰动、成岩作用、人为污染、水体局限、高有机碳通量、Fe、Mn氧化物循环等因素通过影响氧化还原敏感元素在沉积物中的富集与迁移,从而影响氧化还原敏感元素指标的应用,应剔除有机质吸附与陆源输入等非自生部分的影响,结合各种指标互相印证,综合判别水体氧化还原状态。     

冈底斯岩浆弧东端石榴斜长角闪岩的晚白垩世岩浆与变质作用记录及构造意义

冈底斯岩浆弧位于青藏高原拉萨地体南部,形成在新特提斯洋向北俯冲的安第斯型造山和印度与欧亚大陆碰撞的喜马拉雅型造山过程中,是研究青藏高原中-新生代构造演化的理想地区。本文对冈底斯岩浆弧东端石榴斜长角闪岩进行了岩石学、相平衡模拟以及锆石U-Pb年代学研究。石榴斜长角闪岩主要由石榴石、角闪石、斜长石、绿帘石、白云母和石英组成,含少量金红石和钛铁矿,具有基性岩浆岩的化学成分。相平衡模拟结果表明,石榴斜长角闪岩经历了高压麻粒岩相变质作用和部分熔融,峰期变质作用的温度和压力条件为～820℃和～1.67GPa,形成深度相当于55km。石榴斜长角闪岩中的锆石具有继承的岩浆核和变质边。锆石岩浆核具有条带状环带,相对高的HREE含量(平均值为1150×10~(-6))和高的Th/U比值(0.51～0.95),给出了90.4±1.7Ma(MSWD=0.32)的原岩结晶年龄。锆石的变质边不具环带,具有较低的HREE含量(平均值为58.5×10~(-6))和低的Th/U比值(0.29～0.40),给出了86.7±5.7Ma(MSWD=0.15)的变质年龄。本文研究结果表明,冈底斯岩浆弧东端晚白垩世辉长岩经历了近侵入同期的高压高温变质作用和部分熔融,大体积幔源岩浆的底垫和增生导致岩浆弧发生了显著的新生地壳生长和加厚。