X Per新发射相的不寻常变化

对ＸＰｅｒ新发射相连续四年的光学光谱和近红外光度监测结果，ＸＰｅｒ近两年的变化不同寻常，主要表现以下两点：（１）尽管它的光学光度Ｖ星等只恢复至失去气壳前的亮度，但Ｈａ发射线等值宽度和近红外，Ｊ，Ｈ和Ｋ光度地超过了历史记录的最大值，分别达到了１６．３４Ａ和５．３＾ｍ，５．３＾ｍ和５．１＾ｍ，表明ＸＰｅｒ新发射相气南的密度和尺度较都大，（２）我们首次观测到ＸＰｅｒ近红外光度和Ｈα发射线等值宽度变化趋势     

Cepheus OB3巨分子云复合体成块性质的研究

根据文[1]中图1（a）和图1（b），分别对CepB和CepF进行成图处理，得到了它们的强度分布图和速度分段积分等高图，通过对这些强度分布图和速度分段积分等高图的分析和研究，也得到了CegheusOB3巨分子云复合体是成块的，并且这些块是没有被自引力束缚的，同时还得到了CepB和CepF的外流的动力学时标。     

H-alpha太阳全日面像数据管理系统的建立

云南天文台的H-alpha太阳色球望远镜每天的数据量约有2G bytes，大量数据带来了使用上的不便。因此，实现数据的查询和共享成为了一个相当重要的问题。为此，试图通过建立H-alpha数据的管理系统，实现对工作流程的改进，完成对数据的检索、在线浏览和远程下载。在WindwsXP操作系统和MysQL数据库管理系统的平台上，利用JAVA语言和JSP技术开发了一个基于浏览器／服务器模式的原型系统，可以完成对数据的压缩存储，实现数据的检索、实时浏览、删除(需要相应权限)和下载等功能。     

日冕电子加速的诊断—多频射电高时间分辨率观测结果

一个太阳耀斑约含数千个微耀斑［１］，每个微耀斑以热的，低频波和加速粒子的形式释放能量。耀斑期间大部分能量的释放是通过电子加速转移的结果，然而电子加速是在耀斑前相开始，并在整个耀斑持续期间继续保持。在耀斑发展的不同相期间伴有各种各样的射电辐射现象（及其它波段共生现象），多波段射电观测和比较可以给出有关电子加速过程和耀斑自身发展的重要信息，尤其可检测加速开始的时间和频率部位（目前仍为太阳物理的前沿）。微耀斑能量的瞬时释放可能是引起不同类型快速精细结构的原因，射电毫秒级尖峰辐射是起因于连续能量释放的证据，其辐射源位于或靠近能量释放区［２］，公认射电辐射的快速结构是日冕电子束的特征信号［３，４］，所以今后使用高时间和高频率分辨率的宽带频谱仪同时观测可详细地探测加速过程，从而对预耀斑的加热和初始能量释放，耀斑的逐步建立和演化都具有重要意义。本文介绍几个典型事件，包括射电尖峰脉冲辐射，类尖峰辐射和短时标漂移结构     

Blazar 的X射线谱性质

从Donato文献中选择了一个含有69个Blazar的样本，样本中每个源有多个X射线辐射流量数据，用该样本研究了流量密度和谱指数之间的关系，以及研究了三类源（HBL，LBL，FSRQ）的红移和谱指数的分布。结果表明：对于HBLs，谱指数和流量密度之间有一个较好的反相关关系存在，而对于LBLs和FSRQs却没有相关。因此认为HBL的X射线是同步辐射所致，而LBL和FSRQ的X射线辐射较为复杂可能是同步自康普顿过程导致。HBL显示软X射线谱，而FSRQ显示硬X射线谱，LBL居中。在谱图中HBL位于近端，rSRQ位于远端，LBL居中。     

盾牌座δ型变星4CVn的多重非径向脉动振幅变化

对非径向脉动δＳｃｕｔｉ（盾牌座δ）型变星４ＣＶｎ的最新光电测光观测，证实了其振幅和周期的长期缓慢变化．两种多重频率分析方法都一致确认出已知７个频率中的５个（ｆ１，ｆ２，ｆ３，ｆ５，ｆ７）．观测还发现三个可疑频率．目前主频的振幅和十几年前的一样，基本保持不变，可能正处于向最大振幅变化的增加阶段或者处于刚过极大的下降段．其它四个频率的振幅都不同程度地变大．ｆ２，ｆ３和ｆ５的振幅增幅分别为６３％，２５％和１２０％，尤其是ｆ７，从上次的０变为０．００９ｍａｇ．频率分析显示除主频ｆ１几乎未变外，其它频率缓慢变化：ｆ２和ｆ７约减小０．０８％；ｆ３减小０．１４％；ｆ５增加０．０３％．用Ｂｌａｚｈｋｏ效应和不同非径向脉动模式之间的共振解释振幅和周期变化的合理性，尚需进一步从观测上检验．     

射电源AO 0235＋164不同波段之间的相关时延分析及谱指数演化

详细介绍了由Edelson和Krolik提出的离散相关分析方法，该方法比较适合于因天文观测的不规则性而引起的时间分布不均匀的不同波段之间流量的相关分析，取两种极端的情况（完全相关和完全不相关）对该方法进行了测试，结果表明这是一种比较切实可行的方法。利用它，对AO0235＋164在4个波段上流量变化作相关性分析，结果表明，AO 0235＋164在5GHz,8GHz,14.5GHz和光学BI皮段的辐射之间存在着明显的相关性，高频波段的流量变化早于低频波段的流量变化，表明这些波段的辐射（从射电到光学）可能来源于相同的辐射机制，或者辐射是相关的，另外发现，谱指数随着时间而发生变化，这种变化在5GHz 8GHz和14．5GHz之间多表现为逆谱的形式，种种迹象表明AO 0235 164的射电爆发可能是和激波的形成有关，多波段的频谱分析和频谱演化研究可能是揭示这种关系的有效途径。     

中子星的热演化和磁衰减

本文研究了中子星的热演化、自转演化和磁场演化的相互影响．考虑了一个自洽模型：中子星因磁偶极辐射而自转减慢，在内部产生某些加热过程，中子星磁场通过壳层的欧姆耗散来衰减．结果表明，磁场衰减提高了加热过程的重要性；相反，加热效应减慢了磁衰减．因此可以得出，中子星的热、自转和磁场也许不是独立演化的．不仅如此，这些演化与初始条件有关，因此，人们也许可以从射电和Ｘ射线观测对脉冲星年龄、初始磁场和周期给出某些限制．     

卫星轨道预报的一种分析方法

人造地球卫星的轨道预报是空间环境监测和实时跟踪测量中一个重要环节，由于监测对象众多，要求精度也不太高，通常采用分析法预报．在已有分析法得到t时刻平均根数的基础上给出一种轨道预报方法，由t时刻的平均根数给出该时刻卫星的位置和速度，在此基础上将地球非球形引力摄动的周期项直接用卫星直角坐标的位置和速度分量表示，这样可以避免在计算轨道根数变化的周期项时出现的奇点问题，从而对根数的选择无特殊要求，可适用于各种轨道，简化预报程序和相应的软件，提高预报效率。     

彗木相撞的不可压缩分层流体模型

提出了一个彗木相撞的线性模型．在这个模型中，将木星大气看作是一个分层的、不可压缩和无粘滞的流体层，而与撞击相联的引力波则由一个初始冲力所造成．采用初始冲压P(r，z，0)代替初始表面形变作为初始条件．发现这种做法使得问题的数学处理更加方便，特别是在计算流体粒子的垂直位移和摄动势能方面，后者可以表为P(r，z，0)的有限傅立叶正弦和余弦变换．导出了一个联系彗星碰撞参数、木星大气参数和所设初始冲力之间的关系式．还对两种P(r，z，0)的假设形式分析地导出表面波波高．     

A new red variable star in the globularcluster M4

G302 = L3107 is a red star located at the lowest end of the red giant branch of the globular cluster M4. According to its location on the C-M diagram, G302 may be a cluster member. No proper motion or radial velocity determinations are available up to date.

We discovered that C302 is a new variable star with a main period of 1.24719 day and a peak to peak amplitude of about 0.3 mag in V. It may have a second period of 2.38249 day with an amplitude of about 0.05 mag. If it is a cluster member, then there will be interesting implications for the the theory of stellar evolution.     

Another new small-amplitude red variable star with period of about one day in the globular cluster M4

A66 is a red star located at the lowest end of the red giant branch (near the top of the sub-giant branch) of the globular cluster M4. According to its location on the GM diagram, A66 may be a cluster member. No proper motion and radial velocity determinations are available up to date.

We discovered that A66 is a small-amplitude new variable star with a period of about one day and the peak to peak amplitude is about 0.05 mag in V.

However, if its membership can be confirmed by proper motion and radial velocity determinations, the cause of light variation may be not pulsation. This is because according to Xiong's theory, a red star at such low luminosity can not pulsate at a period longer than 0.1 day. Then other causes such as EW type eclipsing variable star or rotation of a spotted star might be responsible. Otherwise A66 is not a cluster member.     

G328: A Small-Amplitude Red Variable with a Period Near One Day

G328 = A65 = L3314 (V = 13.83, B-V = 1.91) is a field star in the direction of the globular cluster M4. If we take E(B - V) = 0.40, then its (B - V)0 = 1.51, corresponding to a spectral type of K5III if it is a giant star; or of dM2 if it is a dwarf. Observations at both the MSSSO and Yunnan Observatory have shown that G328 is a new variable with peak to peak amplitude - 0.05 mag in V. While it is not unusual for so red a star to be a variable, special attention must be paid to its short period of about one day. If the variability is due to pulsation, the spectral type and luminosity as well as effective temperature should be determined in order to compare it with Xiong's theory.     

Variable Star Status of Two Stars:V204 and I-I-39 in M3

The star I-I-42 (=vZ1390),a cluster member in M3,located near the red edge of the instability strip of the horizontal branch,was discovered by Roberts and Sandage as a low amplitude variable,it was designated as V204 in the "second catalogue of variable stars in globular clusters",but its coordinates given in all versions of this catalogue are wrong since 1955. We argue that V204 is indeed a low amplitude HB variable star,located near to the red edge of the instability strip,with a period of 0.74785d and an amplitude of about 0.04mag in V . We also find that the red cluster member star I-I-39 is a low amplitude variable with a period of 1.16d and amplitude of about 0.03mag in V which might be pulsating at the second overtone.     

G298 – A New Candidate γ Doradus Star in the Direction of the Globular Cluster M4

G298 = L3216 (V = 12.68, B?V = 0.59) is a field star in the direction of the globular cluster M4. It was used as one of our comparison stars in the past, now it is shown that G298 is a new γ Dor variable star with a period of 1.03099 day and peak to peak amplitude of about 0.02 mag in V. Its spectral type is F2 (IV ?).     

Activity history of the spotted rotating star HII 296 in the Pleiades

Observations of the spotted rotating G8 V star HII 296, a member of the Pleiades cluster, are presented. The star has exhibited stable periodic brightness variations for several years. The apparent rotation period of the star in our observations was 2.53 and 2.58 days. The shape and amplitude of its light curve changed from year to year. During our observational monitoring from September to November 2012, we recorded an almost complete absence of brightness variations in September. A rapid (within a few weeks) and manyfold increase in the brightness variability amplitude was observed in October and November 2012. The changes in the rotation period, amplitude, and shape of the light curve suggest an intense relative motion of spots in latitude and longitude.     

Automated classification of variable stars for All-Sky Automated Survey 1–2 data

With the advent of surveys generating multi-epoch photometry and the discovery of large numbers of variable stars, the classification of these stars has to be automatic. We have developed such a classification procedure for about 1700 stars from the variable star catalogue of the All-Sky Automated Survey 1–2 (ASAS 1–2) by selecting the periodic stars and by applying an unsupervised Bayesian classifier using parameters obtained through a Fourier decomposition of the light curve. For irregular light curves we used the period and moments of the magnitude distribution for the classification. In the case of ASAS 1–2, 83 per cent of variable objects are red giants. A general relation between the period and amplitude is found for a large fraction of those stars. The selection led to 302 periodic and 1429 semiperiodic stars, which are classified in six major groups: eclipsing binaries, 'sinusoidal curves', Cepheids, small amplitude red variables, SR and Mira stars. The type classification error level is estimated to be about 7 per cent.     

球状星团M3水平支脉动不稳定带红边界附近的小变幅变星

半个世纪以前,Ｒｏｂｅｒｔｓ 和Ｓａｎｄａｇｅ 在验证Ｓｃｈｗａｒｚｓｃｈｉｌｄ 的理论发现时,在水平支ＲＲＬｙｒａｅ 变星缺口段的红端发现了两颗小变幅的变星。当时定不出类型,标以“？”。以后Ｓａｎｄａｇｅ 在做ＲＲ Ｌｙｒａｅ 变星统计研究时,竟不加解释地当作ＲＲａｂ 型星处理。半个世纪之间,没有人对这颗星的反常加以注意。我们用国内的ＣＣＤ 观测,又发现了一颗类似的小变幅变星,但变幅更小,周期更长。这颗星与以前发现的两颗一起,似乎构成ＲＲ Ｌｙｒａｅ 星的又一个次型。现有的变星脉动理论还不能对之加以解释。我们预计,这将再一次推动脉动理论发展。     

Open cluster membership probability based on K-means clustering algorithm

In the field of galaxies images, the relative coordinate positions of each star with respect to all the other stars are adapted. Therefore the membership of star cluster will be adapted by two basic criterions, one for geometric membership and other for physical (photometric) membership. So in this paper, we presented a new method for the determination of open cluster membership based on K-means clustering algorithm. This algorithm allows us to efficiently discriminate the cluster membership from the field stars. To validate the method we applied it on NGC 188 and NGC 2266, membership stars in these clusters have been obtained. The color-magnitude diagram of the membership stars is significantly clearer and shows a well-defined main sequence and a red giant branch in NGC 188, which allows us to better constrain the cluster members and estimate their physical parameters. The membership probabilities have been calculated and compared to those obtained by the other methods. The results show that the K-means clustering algorithm can effectively select probable member stars in space without any assumption about the spatial distribution of stars in cluster or field. The similarity of our results is in a good agreement with results derived by previous works.     

UBV photometry of X-ray system with M2 III type red giant V934 her (4U 1700+24)

V934 Her is a detached system, consisting of a cool giant and a neutron star. The neutron star accretes matter fromthe stellarwind of the giant.Multicolor photoelectric observationsmade in 1997–2011 revealed a 415-day period, close to that, discovered spectroscopically from radial velocities. This period is considered to be the orbital period of orbital motion of the neutron star around the red giant. The wave with this period in the U-band has the largest amplitude 0^m.12. We also detected multiperiodic pulsations of the red giant. The light curve in the V -band is dominated by a pulsation wave with the period of 28.82 days and the amplitude of 0^m.10.