强矿震地球物理过程及短临阶段预测的研究

基于中尺度地震实验场高密度数字地震和前兆台网对抚顺老虎台矿两次强矿震进行连续的现场观测,用地震学方法和小波工具分析强矿震孕震过程采集到的数据,提取短临阶段的异常信息;用区域强震震源机制解、强矿震的震源机制解、极近场震源调查、震源高精度定位、现场绝对地应力测量、三维有限差分数值试验方法,分析强矿震的孕震应力场环境和震源机制;通过定量观察采矿与矿震活动的相关性,分析强矿震的直接诱发原因．提出地质构造环境、地应力场和采矿活动共同作用诱发强矿震的机理和局部应力场在孕育该震过程起主导作用、卸荷重力应力场抑或耦合了高压瓦斯的膨胀起主要诱发作用的观点;发现煤炭深部开采条件下,矿震和瓦斯存在密切的相关性,有可能存在一种开采卸荷和高压瓦斯气体膨胀耦合作用诱发的新型矿震——卸胀耦合型矿震;提取到震前短临阶段存在的b值、η值、频次、波速比等可信的地震学异常和定点潮汐形变前兆异常,对异常信息的提取方法和强矿震短临阶段的预测进行了探讨．     

Research on the Method of Orbit Determination Based on the Self-adaptive Stable Least p-norm Estimate

The traditional least square estimation (LSE) method for orbit determination will not be optimal if the error of observational data does not obey the Gaussian distribution. In order to solve this problem, the least p-norm (Lp) estimation method is presented in this paper to deal with the non-Gaussian distribution cases. We show that a suitable selection of parameter p may guarantee a reasonable orbit determination result. The character of Lp estimation is analyzed. It is shown that the traditional Lp estimation method is not a robust method. And a stable Lp estimating based on data depth weighting is put forward to deal with the model error and outlier. In the orbit determination process, the outlier of observational data and coarse model error can be quantitatively described by their weights. The farther is the data from the data center, the smaller is the value of data depth and the smaller is the weighted value accordingly. The result of the new Lp method is stabler than that of the traditional Lp estimation and the breakdown point could be up to 1/2. In addition, the orbit parameter is adaptively estimated by residual analysis and matrix estimation method, and the estimation efficiency is enhanced. Finally, by taking the Space-based Space Surveillance System as an example and performing simulation experiments, we show that if there are system error or abnormal value in the observational data or system error in satellite dynamical model and space-based observation platform, LSE will not be optimal even though the observational data obeys the Gaussian distribution, and the orbit determination precision by the self-adaptive robust Lp estimation method is much better than that by the traditional LSE method.     

Analysis of Land Water Storage in Southwest China Based on GRACE Data

The inversion of the variation in the land water storage in Southwest China is carried out by taking advantage of the data obtained by the earth gravity satellite GRACE (Gravity Recovery and Climate Experiment) for 64 months from January 2005 to April 2010. The result shows that by selecting an appropriate Gauss radius (R = 600 km) and taking the average gravitational field of the adopted data as the back-ground gravitational field, the land water storage in Southwest China inverted on the basis of the GRACE data reflects the drought in Southwest China at the beginning of 2010 very well.     

太阳硬X射线成像望远镜模拟研究

调制准直器型太阳硬X射线成像望远镜是目前较为通用的太阳观测设备.空间调制望远镜是基于中心轴不旋转的望远镜,适用于3轴稳定的卫星.针对我国可能的太阳观测计划,给出并比较了两组空间调制望远镜的配置方案,然后利用GEANT4高能物理通用软件模拟实际光子的计数情况,使用MATLAB实现图像重建.比较模拟光子计数得到的重建图与几...     

CDFS天区中喑蓝星系的测光红移研究

从COMBO-17数字巡天数据里,选择了CDFS(Chandra Deep Field South)天区中1231个测光红移在0.1～0.3之间的暗蓝星系作为样本,研究了这些星系分别在只有光学波段和光学加近红外波段数据情况下做测光红移得到的红移分布,以及这些星系在静止参考系下的能谱分布(Spectral Energy Distributions,SEDs)特征.结果表明有183个星系在利用光学加近红外波段数据做测光红移时得到的红移大于1.2,它们的误差为0.046,提高测光的信噪比也有利于区分这类被光学波段误认为低红移的星系.这些暗蓝星系中高红移星系的观测近红外流量相对于光学流量有上升的趋势,而低红移星系的观测近红外流量相对于光学流量有下降的趋势.     

非线性相对运动下空间碎片碰撞概率计算的研究

空间目标碰撞概率的计算是航天器进行空间碎片预警和规避机动的基础.为了简化计算,目前国内外在计算碰撞概率问题过程中大多基于线性相对运动的条件,将三维碰撞概率计算积分问题简化为位置误差概率密度函数在圆域内的二维积分问题.但是当空间目标相对运动速度较小时,这种线性运动条件不再成立,就需要在真实的非线性相对运动状态下重新考虑碰...     

幂律电子谱轫致辐射积分的快速计算

SSW(Solar SoftWare)的能量电子产生X光子的轫致辐射积分计算发展到版本2时,其性能相比初始的版本1提高很多.在版本2的基础上,对这个积分进一步改进.通过对比几种轫致辐射积分方案,结果显示,最终的方案性能上比版本2可以快约2～5倍.在积分的精确性上比版本1及版本2均改进了很多,在缺省的积分控制精度下也不再产生光子谱的尖刺现象.而且,积分耗时不再敏感于积分上限取值.由于积分性能的提高,使得利用精确的轫致辐射截面计算轫致积分成为可能.结果显示,用精确轫致辐射截面比先前的近似截面积分的结果光子流量略小(≤4%),积分时间大约比先前使用近似截面多30%.     

Relaxation of protostellar accretion shocks using the smoothed particle hydrodynamics

It is believed that protostellar accretion disks are formed from nearly ballistic infall of molecular matter in rotating core collapse. Collisions of this infalling matter leads to formation of strong supersonic shocks, which if they cool rapidly, result in accumulation of that material in a thin structure in the equatorial plane. Here, we investigate the relaxation time of the protostellar accretion post‐shock gas using the smoothed particle hydrodynamics (SPH). For this purpose, a one‐dimensional head‐on collision of two molecular sheets is considered, and the time evolution of the temperature and density of the post‐shock region simulated. The results show that in strong supersonic shocks, the temperature of the post‐shock gas quickly increases proportional to square of the Mach number, and then gradually decreases according to the cooling processes. Using a suitable cooling function shows that in appropriate time‐scale, the center of the collision, which is at the equatorial plane of the core, is converted to a thin dense molecular disk, together with atomic and ionized gases around it. This structure for accretion disks may justify the suitable conditions for grain growth and formation of proto‐planetary entities (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Mining the CFHT Legacy Survey for known Near Earth Asteroids

The Canada‐France‐Hawaii Legacy Survey (CFHTLS) comprising about 25 000 MegaCam images was data mined to search for serendipitous encounters of known Near Earth Asteroids (NEAs) and Potentially Hazardous Asteroids (PHAs). A total of 143 asteroids (109 NEAs and 34 PHAs) were found on 508 candidate images which were field corrected and measured carefully, and their astrometry was reported to Minor Planet Centre. Both recoveries and precoveries (apparitions before discovery) were reported, including data for 27 precovered asteroids (20 NEAs and 7 PHAs) and 116 recovered asteroids (89 NEAs and 27 PHAs). Our data prolonged arcs for 41 orbits at first or last opposition, refined 35 orbits by fitting data taken at one new opposition, recovered 6 NEAs at their second opposition and allowed us to ameliorate most orbits and their Minimal Orbital Intersection Distance (MOID), an important parameter to monitor for potential Earth impact hazard in the future (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Horizon synthesis for archaeo‐astronomical purposes

In this paper I describe a simple numerical procedure to compute synthetic horizon altitude profiles for any given site. The method makes use of a simplified model of local Earth's curvature, and it is based on the availability of digital elevation models describing the topography of the area surrounding the site under study. Examples constructed using the Shuttle Radar Topographic Mission (SRTM) data (with 90 m horizontal resolution) are illustrated, and compared to direct theodolite measurements. The proposed method appears to be reliable and applicable in all cases when the distance to the local horizon is larger than ∼10 km, yielding a rms accuracy of ∼0.1 degrees (both in azimuth and elevation). Higher accuracies can be achieved with higher resolution digital elevation models, like those produced by many modern national geodetic surveys (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)