2002年7月23日X射线耀斑的RHESSI和TRACE观测物理图像

通过对比分析TRACE195A和RHESSI的X射线及Ha的图像，发现2002年7月23日的X4.8级耀斑的主体是一个典型的双带耀斑，它的Ha及TRACE195A的图像都显现出明显的双带耀斑特征，TRACE195A的像还呈现一个环拱结构，其环拱的足点与TRACE的亮带并不重合，但TRACE的亮带与X射线像的位置对应很好．在耀斑极大时刻附近，大于38keV的X射线像呈现一个低的环跨在TRACE的双带上，X射线环的顶点及两足点尤其明显，在这个低的环上方，还存在一个在低能量段明显的X射线日冕源，对该耀斑的空间结构及演化特征作了描述，还简单地讨论了一个可能的理论解释．     

Robert E. Horton's perceptual model of infiltration processes

Robert E. Horton is best known as the originator of the infiltration excess overland flow concept for storm hydrograph analysis and prediction, which, in conjunction with the unit hydrograph concept, provided the foundation for engineering hydrology for several decades. Although these concepts, at least in their simplest form, have been largely superseded, a study of Horton's archived scientific papers reveals that his perceptual model of infiltration processes and appreciation of scale problems in modelling were far more sophisticated and complete than normally presented in hydrological texts. His understanding of surface controls on infiltration remain relevant today. Copyright © 2004 John Wiley & Sons, Ltd.     

A hybrid simulation study of magnetic reconnection in anisotropic plasmas

The process of magnetic reconnection in anisotropic plasmas is studied numerically using a 2-dimensional, 3-component hybrid simulation. The results of the calculation show that, when the plasma pressure in the direction perpendicular to magnetic field is larger than that in the parallel direction (e.g. P/P = 1.5), instability may greatly increase, speeding up the rate of reconnection. When P is smaller than P, (e.g., when P/P = 0.6), fire hose instability appears, which will restrain the tearing mode instability and the process of magnetic reconnection.     

Observation of a type of sporadic solar mass ejection and its physical interpretation with numerical simulation

Seven mediated and small ejective events on the sun observed at Ganyu Observing Station of Purple Mountain Observatory in 2000 are investigated. It is found that they were not accompanied by brightening. Their lengths were in the range 1–2.5×10⁴ km, their widths, 3–5×10³ km, and their lifetimes, 3–7 minutes. They were produced at places of weak magnetic fields and far away from large sunspots. These ejections are interpreted by numerical simulation with 1-D hydrodynamic equations of flow along magnetic arcs. As demonstrated by the results, they are different from the spicules and surges simulated by Suematsu et al. and Shibata et al. They are not matter with photospheric or chromospheric densities pushed by shock waves or rebound shock waves toward the solar corona, rather, they are ejections formed by continuous matter flows after magnetic reconnection. After evolving for about 5 minutes, they can attain a stationary hydrodynamic state.     

光子计数式光电测光系统数据采集和控制软件

本文报告了数据采集和控制软件ＣＭＵＯＰＰＳ的研制情况，这个软件是云南天文台密近双星研究组为泰国清迈大学天文台研制的光子计数式光电测光系统的专用配套软件。文中给出了硬件接口的性能及软件和硬件握手的方案，介绍了软件的总体概况，还说明了软件的使用环境和使用方法。最后给出了实验室测试和试观测过程中软件的运行情况及结果。     

太阳运动IV型射电爆发的相干辐射模型

为解释太阳运动IV型射电爆发的相干辐射机制提出一个理论模型．从耀斑中产生的高能电子，可以被扩展上升的太阳磁流管俘获．在磁流管顶部，这些高能电子的速度分布形成为类束流速度分布，激发束流等离子体的不稳定性，并且主要直接放大O模电磁波．不稳定性增长率敏锐地依赖了日冕等离子体参数，fpe／fce和射束温度Tb，这能定性解释在太阳运动IV型射电爆发中观测到的高亮温度和高偏振度，以及宽频谱的特性．     

对一个太阳风暴及其行星际和地磁效应的研究

对一个爆发于2014年1月7日的太阳风暴进行了研究,通过对太阳活动的多波段遥感观测—来自于太阳动力学天文台(Solar Dynamics Observatory,SDO)以及太阳和日球天文台(Solar and Heliospheric Observatory,SOHO),分析了耀斑和日冕物质抛射(coronal mass ejection,CME)的爆发过程.通过地球同步轨道环境业务卫星(Geostationary Operational Environmental Satellites,GOES)对高能质子以及日地L1点的元素高级成分探测器(Advanced Composition Explorer,ACE)对当地等离子体环境的就位观测,分析了伴随太阳风暴的太阳高能粒子(solar energetic particle,SEP)事件和行星际CME(ICME)及其驱动的激波.通过地面磁场数据分析了该太阳风暴对地磁场的影响.研究结果表明:(1)耀斑脉冲相的开始时刻和CME在日面上的抛射在时序上一致.(2)高能质子主要源于CME驱动的激波加速,并非源于耀斑磁重联过程.质子的释放发生在CME传播到7.7个太阳半径的高度的时刻.(3)穿过近地空间的行星际激波鞘层的厚度和ICME本身的厚度分别为0.22 au和0.26 au.(4)行星际激波和ICME引起了多次地磁亚暴和极光,但没有产生明显的地磁暴.原因在于ICME没有包含一个规则的磁云结构或明显的南向磁场分量.     

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Linear Correlations between Peak Frequency of Gyrosynchrotron Spectrum and Photosphere Magnetic Fields

The gyrosynchrotron spectra are computed in a nonuniform magnetic field case, taking into account the self-and gyroresonanceabsorption. It is found that the peak frequency νp of the gyrosynchrotron spectrum systematically increases with the increasing photosphere magnetic field strength B0 and increasing viewing angle θ. It is also found for the first time that there are good positive linear correlations between νp and B0, and between log νp and log θ, with linear correlation coefficient 0.99 between νp and B0 and 0.95 between log νp and log θ. We apply the correlations to analyze two burst events observed with OVSA and find that the evolution tendencies of the photosphere magnetic field strength B0 estimated from the above expression are comparable with the observational results of SOHO/MDI. We also give a comparison of the diagnostic results of coronal magnetic field strength in both uniform and nonuniform source models.     

太阳暗条活动的周期性研究

运用法国巴黎默东天文台记录的暗条目录资料构造了一个时间精度为每天的暗条数目序列,选用Scargle周期图和Morlet小波变换两种周期方法研究了这个序列的周期性,发现其存在4个显著的周期,它们分别是1557天、1141天、795天和367天,详细分析了这些周期的时变特征,并简单讨论了其中个别典型周期的相位、物理机制和相互关系．