短周期激变变星周期分布的新统计

我们对周期小于周期分布空缺段的激变变星，重新进行了周期分布统计，使用了比Ｗａｒｎｅｒ等人更多，更新的资料，统计中发现一个ＡＭＨｅｒ型ＣＶｓ：ＧＲＵＶ１偏离了Ｗａｒｎｅｒ等人的统计结果，我们给出了ＣＶＳ新的周期分布图和相应于此分布的随机概率。虽然结果与Ｗａｒｎｅｒ等人的不同，但周期分布同磁场仍呈现一定的相关性，磁激变变星与非磁激变变星同样显示出成团趋势。     

激变变星中的快速光变

文中综述了激变变星中快速光变的研究进展，讨论了闪变，相干振荡和准周期振荡的观测特征和可能的产生机制。     

激变变星中的白矮星

仅在过去的10年中,由于采用了地面和空同时的光谱观测激变变星中正处于吸积过程的白矮星,在激变变星（CV）的研究方面出现了全新的途径。这些光谱探测开拓了恒星包层、角动量团儿CV演化中吸积物理学研究的新前没中。这篇评论包括了激变变星中的白矮星研究的方方面面：（1）表面温度;（2）吸积加热和冷却的不;(3)在高度倾斜的CV中吸收幕帘（盘的上面的大气）的影响和特点;（4）白矮星光球的化学丰度;（6）吸积带;（7）吸积的模拟。     

双星统计演化及激变变星的形成

介绍了双得统计演化的方法和手段,并对激变星的形成进行了Monte-Carlo模拟,模拟显示,激变变星的诞生度、白矮子星质量分布、轨道周期分布的理论结果与观测结果保持一致。另外,还研究了激变变星的形成与模型参量之间的关系,这些参量包括公共包层抛射效率、双星初始质量比分布、年龄、金融丰度等。     

激变变星中吸积盘的边界问题

边界层是介于吸积盘和吸积星之间的非常狭窄的区域，在该区域中随着盘物质接近星面，它的角速度从开普勒角速度下降至恒星自转角速度。边界区因释放的能量接近吸积光度的一半，并且为确定吸积盘微分方程提供内边界条件而显示出它的重要性。本文综述了激变变星中吸积盘边界层的研究进展。     

激变变星的长期演化

介绍激变变星长期演化的基本概念和标准模型,及辐照效应对激变变星长期演化的影响。     

激变变星的多波段研究（Ⅰ）

最近十年来，无论是在观测上还是在理论上，人们对激变变星的认识都取得了巨大进展。本文从射电，红外，可见光三个波段对激变变量的观测现象，如流量分布，光变曲线，驼峰现象和闪烁现象，以及对这些观测现象的理论解释作一简单介绍。     

间隙时间序列谱分析方法的检验及其在激变变星短周期振荡分析中的…

本文对具有或长或短间隙（ｇａｐ）的时间序列的谱分析方法进行研究，给出递推公式，并且用模拟信号进行检验，证实这个方法的可靠性，并把它应用到激变变星Ｖ７９５Ｈｅｒ和激变前景为星ＨＷ，Ｖｉｒ的短周期振荡分析中，结果表明这两颗变星都有明显的闪变，在Ｖ７９５Ｈｅｒ中还存在周期为２６５．９１ｓ和１１６．７０ｓ的振荡。     

CCD Time-Resolved Photometry of Four Newly Discovered CVs

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X-ray observations of non-magnetic CVs in the ASCA era and beyond

Our ability to study the hard X-ray emission in non-magnetic CVs has improved dramatically within the last decade. We review the important results on X-ray eclipses and dips, the current state-of-the-art in the modeling of X-ray spectra of CVs, then present some recent results on the hard X-ray emission from high accretion rate non-magnetic CVs. These results point to potential areas of conflict with accretion disk theories: the fate of the inner disk in quiescence, and the amount of material above the orbital plane. We conclude with some speculations on where near-future X-ray missions might take this field over the next decade.     

Short-Period Features of the Interplanetary Plasma and Their Evolution

The solar wind plasma exhibits many features of the solar surface passed on to the interplanetary medium as temporal variations due to the solar rotation. The yearly average values of solar wind velocity, and geomagnetic index A _p during 1965–1999 were found to exhibit long period evolution. They were found to peak around the declining phase of each solar cycle. While the solar wind velocity peaks around the second half of the declining phase, the IMF field strength increases around the first half of the declining phase of each solar cycle. The power spectrum of these parameters shows peaks around 37-day, 30-day, 27-day, 13.5-day, 9-day, and 7-day periods. The temporal evolution of the power spectrum of the solar wind plasma parameters and the geomagnetic activity index A _p are also studied in detail and presented with the help of contour graphs. These studies indicate that the strength of the quasi-periodicities in the interplanetary medium evolves with time.     

短周期彗星表面水冰升华分布研究

彗星是太阳系遗留的原始星子,研究彗星彗核的演化对理解太阳系其他天体的形成和演化历史具有重要意义.在太阳的辐射作用下,彗星携带的挥发性成分会发生升华,并带动尘埃运动,造成彗核物质的损失.因此,彗核的升华活动对其表面形貌甚至整体形状演化都会产生影响.从IAU (International Astronomical Union) MPC (Minor Planet Center)获取轨道数据,并考虑了彗核的自转以及进动,利用MONET (Mass lossdriven shape evolution model)形状演化模型对短周期彗星做数值模拟,计算得到了短周期彗星1P/Halley、9P/Tempel 1、 19P/Borrelly、 67P/C-G (Churyumov-Gerasimenko)、 81P/Wild 2和103P/Hartley 2在一个轨道周期内的太阳辐射能量以及表面侵蚀深度的分布,结合其动力学参数讨论了自转、进动和公转等特性对其表面水冰升华分布的影响以及造成南北侵蚀差异的可能性.     

Structure and Dynamics of the Centaur Population: Constraints on the Origin of Short-Period Comets

The origin of Jupiter-family comets is linked to the intermediate stage of evolution through the Centaur region. Thus the structure of the Centaur population provides important constraints on sources of short-period comets. We show that our model of the Oort cloud evolution gives results which are consistent with the orbital distribution of observed Centaurs. In particular, it explains the existence of the large population of Centaurs with semimajor axes greater than 60 AU. The main source for these objects is the inner Oort cloud. Both Jupiter-family and Halley-type comets are produced by Centaurs originating from the Oort cloud. The injection rate for Jupiter-family comets coming from the inner Oort cloud is, at least, not less than that for a model based on the observed sample of high-eccentricity trans-Neptunian objects.     

Long-Term Study of the Starspot Activity on the Eclipsing Short-Period RS Canum Venaticorum Star UV Piscium

We present optical photometry of the short period eclipsing RS CVn system, UV Piscium for the years 1966–1984. After removing the spot effects from the light curves of Vivekananda Rao and Sarma (1981), we analyzed the cleaned data to obtain system parameters. For each light curve, we model the distortion waves in order to study the behaviour of star spots in this system. This revised version was published online in July 2006 with corrections to the Cover Date.     

泊松分布下线性多重回归问题

对一实验数据组进行线性多重回归,如果数据的涨落服从泊松概率分布,常用方法不能给出准确的解。一般地,是假设各泊松分布的形状近似于高斯分布,给出近似解。因此,也存在着人所共知的拟合曲线下的面积亏损问题。本文从最大或然法出发,不加任何假设,严格推导了求解泊松分布线性多重回归的一种方法。按这一方法,“面积亏损”问题在计算精度范围内也得到彻底解决。     

试论行星磁场强度分布的成因

行星磁场强度的分布具有规律性,中间巨行星的强度值大,两侧类地行星和远日行星的强度值小。在类地行星和远日行星中,也是中间行星磁场强度值大,如地球和海王星。两侧行星磁场强度值小,如金星、火星、天王星和冥王星。水星磁场强度值比金星大是因为水星环较早的从A组星云环中分裂出来所致。行星磁场强度大小分布的规律性与星云环级式分裂、环体物质中聚即铁磁性物质较快中聚的规律性一致。所以,铁磁性物质多少,可能是行星磁场强度大小分布的一个主要原因。