Fe~（＋24）、Fe~（＋25）低能态能级结构及K_α、K_β特征线的计算──相对论微扰法

本文采用相对论微扰法处理Ｆｅ（＋２４）系统，利用解析形式的波函数计算其低能态的能级结构及Ｋα、Ｋβ特征线（作为对比，我们也计算了Ｆｅ（＋２５）系统）．通过与现有的Ｆｅ（＋２５）Ｋα线的实验和理论比较，证明我们的方法是准确可信的，而在数学计算上则更加简便。利用这一结果，对小质量Ｘ射线密近双星的Ｆｅ（＋２４）Ｋ特征线进行了简要的定性分析．     

七十年代的X射线天文学

七十年代是X射线天文学空前发展的时代,自美国的“乌呼鲁”卫星成功之后。世界上的各航天大国分别发射了自己的X射线卫星,累积有十几个之多。     

Temporal variations and spectral properties of the Be/X-ray pulsar GRO J1008–57 studied by INTEGRAL

The spin period variations and hard X-ray spectral properties of the Be/Xray pulsar GRO J1008–57 are studied with INTEGRAL observations during two outbursts in 2004 June and 2009 March.The pulsation periods of～93.66 s in 2004and～93.73 s in 2009 are determined.Pulse profiles of GRO J1008–57 during outbursts are strongly energy dependent with a double-peaked profile from 3–7 keV and a single-peaked profile in hard X-rays above 7 keV.Combined with previous measurements,we find that GRO J1008–57 has undergone a spin-down trend from 1993–2009 with a rate of～4.1×10-5s d-1,and could have changed into a spin-up trend after 2009.We find a relatively soft spectrum in the early phase of the 2009 outburst with cutoff energy～13 keV.Above a hard X-ray flux of～10-9erg cm-2s-1,the spectra of GRO J1008–57 during outbursts need an enhanced hydrogen absorption with column density～6×1022cm-2.The observed dip-like pulse profile of GRO J1008–57 in soft X-ray bands could be caused by this intrinsic absorption.Around the outburst peaks,a possible cyclotron resonance scattering feature at～74 keV is detected in the spectra of GRO J1008–57 which is consistent with the feature that was reported in MAXI/GSC observations,making the source a neutron star with the highest known magnetic field(～6.6×1012G)among accreting X-ray pulsars.This marginal feature is supported by the present detections in GRO J1008–57 following the correlation between the fundamental line energies and cutoff energies in accreting X-ray pulsars.Finally we discovered two modulation periods at～124.38 d and～248.78 d using RXTE/ASM light curves of GRO J1008–57.Two flare peaks appearing in the folded light curve had different spectral properties.The normal outburst lasting 0.1 of an orbital phase had a hard spectrum and could not be significantly detected below 3 keV.The second flare lasting ten days showed a very soft spectrum without significant detections above 5 keV.GRO J1008–57 is a good candidate of an accreting system with an equatorial circumstellar disk around the companion star.The neutron star passing the disk of the Be star near periastron and apastron produces two X-ray flares.The soft spectral properties in the secondary flares still need further detailed studies with soft X-ray spectroscopy.     

软伽玛射线再暴体（SGRs）研究进展

对SGRs的主要观测特征－－在软伽玛射线波段的重复爆发及持久性的周期的X射线辐射－－进行了回顾，介绍了SGRs的一些理论模型，其中磁星（具有甚强磁场的中子星）模型较合理地解释了现有的观测事实。     

CygX—3X光子场对γ射线的吸收效应

本文详细讨论了Ｘ射线双星ＣｙｇＸ－３的Ｘ光子场对γ射线的吸收效应，计算结果表明：当ＣｙｇＸ－３的Ｘ光子发射场处于高态时，从致密中子星附近发射的能量为１０＾２－１０＾４ＭｅＶ的γ射线约有６０％被其吸收，吸收过程产生的正负电子的逆Ｃｏｍｐｔｏｎ散射会使出射能量１０－７０ＭｅＶ的 γ射线强度平均增加约５０％，计算的γ射线能谱与实验观测结果基本相符。     

dMe耀星的X射线的辐射

From Einstein Observatory, we know most nearby dM flare stars have X-ray emissions. X-ray flare energy of dM stars is far larger than that of large flares of sun. The corona temperature of dM stars is higher than that of sun. The X-ray flare time scales are several minutes to hours. Star corona heating model for X-ray flares is loop model, which provide a mechanism to convert magnetic energy to heat energy in star corona.Within identification of ROSAT X-ray sources, we found that X-ray source: RX1102.0 4347 corresponds to WX UMa, a dM5e flare star, which is in a nearby visual binary: Gliese 412A B. The binary is very near to earth, 5.38pc, and has high proper motion, 4".54/ year. The binary is also an Einstein X-ray source: 1 E1103.0 4346.In March 27, 1993, we observed WX UMa by CCD BVRI photometry at BAO 2.16m telescope. Magnitudes of the star are: V = 14.56, B-V = 1.95, V-R = 0.97, R-I = 2.06, which are similar to previous observations.From the ROSAT X-ray survey data in November 7-17, 1990, average X     

神舟二号飞船搭载的超软X射线探测器和γ射线探测器初步观测结果

1　科学使命和仪器概况2 0 0 1年 1月 1 0日 ,由中国科学院紫金山天文台研制的超软Ｘ射线探测器和γ射线探测器随神舟二号飞船发射升空并于 1月 1 4日成功投入空间观测 .半年以来 ,两台仪器工作性能稳定 ,遥测参数正常 ,下传的科学数据质量良好 ,完全达到了设计要求 ,并已观测到若干宇宙Ｘ和γ射线爆发事例 ,取得了很有价值的科学数据 .空间天文分系统是载人航天工程空间科学与应用系统的重要组成部分 .它由宽能段、高时间分辨的 3台船载仪器组成 ,并能够相互联合、同步触发观测 .其中 ,超软Ｘ射线探测器的探测能段为 0 .2～ 2ｋｅＶ ,Ｘ射…