Astrophysical motivation for X-ray polarimetry

In this paper I will review the motivation for measuring polarization in the X-ray band from astrophysical sources. Emission models designed to reproduce X-ray spectra can be tested using polarization, and polarization detected in other wavelength bands makes clear predictions as to the X-ray polarization. Polarization is a powerful tool to infer geometrical properties of sources which are too small to be spatially resolved. At the same time, there has been recent progress in instrumentation which is likely to allow searches for X-ray polarization at levels significantly below what was possible for early detectors. This paper will review the history of X-ray polarimetry, discuss some experimental techniques and the scientific problems which can be addressed by future experiments.     

X射线脉冲星导航中的滤波方法分析

X射线脉冲星导航由于需要大量的观测数据来确定天体方位,因此需要较长的滤波周期(500 ～ 1000s),系统的状态方程是非线性的.若采用扩展Kalman滤波(EKF),线性化时会产生较大的高阶截断误差,且Jacobian矩阵不易精确计算,导致定轨的精度较低.文中采用非线性滤波方法- Unscented Kalman 滤...     

聚酰亚胺复合材料的防辐射性能设计

以聚酰亚胺、氧化锆及金属铅粉为主要原材料,制备了聚酰亚胺基复合材料,并进行了X-射线衍射、紫外射线分析.结果表明,聚酰亚胺/氧化锆+金属铅复合材料比纯聚酰亚胺具有更好的X-射线防护性能,耐热性能仍然很好.     

The Swift X-Ray Telescope

he Swift Gamma-Ray Explorer is designed to make prompt multiwavelength observations of gamma-ray bursts (GRBs) and GRB afterglows. The X-ray telescope (XRT) enables Swift to determine GRB positions with a few arcseconds accuracy within 100 s of the burst onset. The XRT utilizes a mirror set built for JET-X and an XMM-Newton/EPIC MOS CCD detector to provide a sensitive broad-band (0.2–10 keV) X-ray imager with effective area of > 120 cm² at 1.5 keV, field of view of 23.6 × 23.6 arcminutes, and angular resolution of 18 arcseconds (HPD). The detection sensitivity is 2×10⁻¹⁴ erg cm⁻² s⁻¹ in 10⁴ s. The instrument is designed to provide automated source detection and position reporting within 5 s of target acquisition. It can also measure the redshifts of GRBs with Fe line emission or other spectral features. The XRT operates in an auto-exposure mode, adjusting the CCD readout mode automatically to optimize the science return for each frame as the source intensity fades. The XRT will measure spectra and lightcurves of the GRB afterglow beginning about a minute after the burst and will follow each burst for days or weeks. Dedicated to David J. Watson, in memory of his valuable contributions to this instrument.     

The entropy in groups – a clue to galaxy formation

The entropy in the hot X-ray gas in groups of galaxies is a fossil of the process of galaxy formation The amount of entropy in these low mass systems considerably exceeds that predicted from structure formation models. To explain these results requires “extra” energy which is a relic of the process of star formation and active galaxy heating. We present new XMM results on the entropy and entropy profiles. These results are inconsistent with pre-heating scenarios which have been developed to explain the entropy floor in groups but are broadly consistent with models of structure formation which include the effects of heating and/or the cooling of the gas. The total entropy in these systems provides a strong constraint on all models of galaxy and group formation, and on the poorly defined feedback process which controls the transformation of gas into stars and thus the formation of structure in the universe.     

Two successive partial mini-filament confined ejections

Active region (AR) NOAA 11476 produced a series of confined plasma ejections, mostly accompanied by flares of X-ray class M, from 08 to 10 May 2012. The structure and evolution of the confined ejections resemble that of EUV surges; however, their origin is associated to the destabilization and eruption of a mini-filament, which lay along the photospheric inversion line (PIL) of a large rotating bipole. Our analysis indicate that the bipole rotation and flux cancellation along the PIL have a main role in destabilizing the structure and triggering the ejections. The observed bipole emerged within the main following AR polarity. Previous studies have analyzed and discussed in detail two events of this series in which the mini-filament erupted as a whole, one at 12:23 UT on 09 May and the other at 04:18 UT on 10 May. In this article we present the observations of the confined eruption and M4.1 flare on 09 May 2012 at 21:01 UT (SOL2012-05-09T21:01:00) and the previous activity in which the mini-filament was involved. For the analysis we use data in multiple wavelengths (UV, EUV, X-rays, and magnetograms) from space instruments. In this particular case, the mini-filament is seen to erupt in two different sections. The northern section erupted accompanied by a C1.6 flare and the southern section did it in association with the M4.1 flare. The global structure and direction of both confined ejections and the location of a far flare kernel, to where the plasma is seen to flow, suggest that both ejections and flares follow a similar underlying mechanism.     

硅基底上外延生长过渡金属硅化物薄膜的研究

过渡金属与硅的接触系统一直被人们所关注,是因为它们在界面处具有肖特基势垒的形成、过渡金属硅化物的外延生长、制作器件的稳定和耐高温等重要性.因此在硅基底上形成金属硅化物薄膜也被广泛应用于半导体工业.对硅衬底上蒸发的Cr、Fe、Mn薄膜进行热处理,通过固相反应法(SPR)制备过渡金属硅化物薄膜,即经过对过渡金属硅化物(薄膜)/Si系统进行各种温度、不同时间的热处理,制备出各种过渡金属硅化物薄膜.对于制成的各种硅化物薄膜,用X射线衍射法(XRD)和软X射线发射分光光谱法(SXES)对它们的组成成分进行了分析和确认.并且,由这两种分析方法表明:各种过渡金属硅化物薄膜在硅衬底上各形成了单一相的均匀层硅化物薄膜.     

双能透照模式下涡轮叶片DR图像融合方法

为了提高单帧涡轮叶片DR(Digital Radiography)图像的信息量,首先在2个不同射线能量下对涡轮叶片进行DR成像,以获取不同厚度区域的质量信息;然后将2幅DR图像进行多分辨率小波分解,以最大局部方差为准则对二者的低频子带图像进行融合,以局部梯度的活性因子为尺度对二者的高频子带图像进行融合;最后基于小波融合系数的逆变换获得最终的融合结果.实验结果表明:基于此方法的涡轮叶片融合DR图像携带了更为丰富的细节信息,从而有利于叶片质量信息的快速、准确判读.      

高能X射线辐照材料的SPH数值模拟

高能脉冲X射线辐照材料时,能量沉积会使材料表层发生气化,并在材料内部形成高压热击波。目前一般采用差分方法对高压热击波过程进行数值模拟。文章尝试采用光滑粒子流体动力学（SPH）方法对X射线辐照材料进行数值模拟,由于材料表层的气化膨胀所致,膨胀后的粒子体积是原来的几十倍甚至上百倍,产生粒子大变形的粒子穿透现象;分析了产生粒子穿透现象的主要原因是气化边界处密度计算公式不合适所致,为此对密度计算公式进行了改进,并开展了基于改进密度计算公式的两种方法的数值模拟,两种方法的计算结果比较一致。