多层次格网模型的近邻指数聚类生态区划算法与实验——以新疆北部地区区划为例

在综合考虑气候、植被、地貌等凶素的基础上,提出一种基于多层次格网模型的最近邻指数-模糊聚类生态区域划分算法(Nearest Neighbor Index Fuzzy clustering,NNI-FIC).该算法采用"自下而上"的方式,首先,利用离散格网单元之间的严格相似性形成区划的核心分区;然后,通过最近邻指数统计分...     

地层不整合遮挡油气藏地质储量计算新方法及其应用

从几何学的观点出发,针对纯油藏和具有气顶的油气藏,采用单储系数、横截面面积与油层横向分布长度三者乘积的方式改进采用单储系数、含油面积与油层厚度三者乘积方式的传统容积法,提出相应的地层不整合遮挡油气藏地质储量计算新公式,并根据油气藏的特点提出水平井钻遇油气藏厚度的预测公式。地层不整合遮挡油气藏的地质储量计算目前主要采用容积法,这类方法不仅计算繁琐,而且不确定因素较多;改进后的新方法计算简单方便,理论性更强,存在的不确定因素显著减少。采用新方法在高青油田高424块高424-1井区进行了实践应用。实践表明:改进的新方法适用于地层不整合遮挡油气藏的地质储量计算及预测水平井钻遇油气藏厚度。     

Simulations for multi-object spectrograph planet surveys

Radial velocity surveys for extrasolar planets generally require substantial amounts of large telescope time in order to monitor a sufficient number of stars. Two of the aspects which can limit such surveys are the single-object capabilities of the spectrograph, and an inefficient observing strategy for a given observing window. In addition, the detection rate of extrasolar planets using the radial velocity method has thus far been relatively linear with time. With the development of various multi-object Doppler survey instruments, there is growing potential to dramatically increase the detection rate using the Doppler method. Several of these instruments have already begun usage in large-scale surveys for extrasolar planets, such as Fibre Large Array Multi Element Spectrograph (FLAMES) on the Very Large Telescope (VLT) and Keck Exoplanet Tracker (ET) on the Sloan 2.5-m wide-field telescope.
In order to plan an effective observing strategy for such a program, one must examine the expected results based on a given observing window and target selection. We present simulations of the expected results from a generic multi-object survey based on calculated noise models and sensitivity for the instrument and the known distribution of exoplanetary system parameters. We have developed code for automatically sifting and fitting the planet candidates produced by the survey to allow for fast follow-up observations to be conducted. The techniques presented here may be applied to a wide range of multi-object planet surveys.     

关于太阳厘米-分米波段频谱日像仪研究进展

摘要：在无线电波段进行射电观测是研究太阳的一个十分重要的手段，不同波段的无线电波反映出不同的特性和状态，其辐射频率与环境参数密切相关。当探测出某一频率上的无线电辐射后，即可诊断源区的电子密度或磁场。因此，建设厘米-分米波段频谱日像仪将首次在该波段上实现同时以高空间、高时间和高频率分辨率观测太阳活动的动力学性质，探测日冕大气。对于太阳物理研究具有重要作用。本文介绍该项目的科学意义、技术方案及预研进展情况。     

基于NiosⅡ嵌入式软核处理器的天文用IRFPA图像采集系统

介绍了一套自主研制的用于地基天文望远镜的，基于IRFPA（红外焦平面阵列）图像采集系统，以及所使用的IRFPA原理、性能特点，着重介绍了IRFPA图像采集系统中以NiosⅡ处理器为核心的电子系统的框架结构方案以及软硬件的设计思想。最后给出了初步的图像采集成像结果。     

A method for aligning the plastic scintillator detector on DAMPE

The Plastic Scintillator Detector(PSD) onboard the DArk Matter Particle Explorer(DAMPE)is designed to measure cosmic ray charge(Z) and to act as a veto detector for gamma ray identification.To fully exploit the charge identification potential of PSD and to enhance its capability to identify gamma ray events, we develop an alignment method for the PSD. The path length of a given track in the volume of a PSD bar is derived taking into account the shift and rotation alignment corrections. By examining energy spectra of corner-passing events and fully contained events, position shifts and rotations of all PSD bars are obtained, and are found to be on average about 1 mm and 0.0015 radian respectively. To validate the alignment method, we introduce artificial shifts and rotations of PSD bars into the detector simulation.These shift and rotation parameters can be recovered successfully by the alignment procedure. As a result of the PSD alignment procedure, the charge resolution of the PSD is improved from 4% to 8%, depending on the nuclei.     

丽江高美古台址和2m级望远镜项目(英文)

自 1992年起云南天文台开始了在云南省西北部的天文选址。丽江高美古最终被选择作为未来中国地基天文光学观测的新址点。并且 ,在国家科技部 ,云南省政府 ,以及中科院的支持下 ,2m级天文望远镜项目在 2 0 0 0年 12月获得立项。在文中 ,我们简要的介绍了高美古台址的情况 ,并给出了 2 .4m望远镜的详细情况 ,以及其他相关情况。     

古本今本《竹书纪年》的天象记载和纪年

对《竹书纪年》记载的天象和纪年进行了初步的分析研究,结果表明,今本《竹书纪年》中新增的天象如日食等,并非汲冢出土佚书的原有内容,而为宋元以后学者所加.     

Heliospheric Observations of STEREO-Directed Coronal Mass Ejections in 2008?–?2010: Lessons for Future Observations of Earth-Directed CMEs

We present a study of coronal mass ejections (CMEs) which impacted one of the STEREO spacecraft between January 2008 and early 2010. We focus our study on 20 CMEs which were observed remotely by the Heliospheric Imagers (HIs) onboard the other STEREO spacecraft up to large heliocentric distances. We compare the predictions of the Fixed-?? and Harmonic Mean (HM) fitting methods, which only differ by the assumed geometry of the CME. It is possible to use these techniques to determine from remote-sensing observations the CME direction of propagation, arrival time and final speed which are compared to in-situ measurements. We find evidence that for large viewing angles, the HM fitting method predicts the CME direction better. However, this may be due to the fact that only wide CMEs can be successfully observed when the CME propagates more than 100^° from the observing spacecraft. Overall eight CMEs, originating from behind the limb as seen by one of the STEREO spacecraft can be tracked and their arrival time at the other STEREO spacecraft can be successfully predicted. This includes CMEs, such as the events on 4 December 2009 and 9 April 2010, which were viewed 130^° away from their direction of propagation. Therefore, we predict that some Earth-directed CMEs will be observed by the HIs until early 2013, when the separation between Earth and one of the STEREO spacecraft will be similar to the separation of the two STEREO spacecraft in 2009??C?2010.