恒星级黑洞(候选体)与太阳耀斑辐射的相似性

本文基于"电子-离子束缚态及其引发核过程"模型(简称"束缚态模型")对Cyg X-1等的X-ray辐射给出X-ray和r-射线等新的产生机制.通过与太阳耀斑光变曲线和能谱比较,得出结论:Cyg X-1、A0620-00、GX339-4、GRSl915+105等的X-ray辐射可能不是"黑洞"的辐射而是星冕的耀斑,这里不需要黑洞.     

氢气辉光放电的非伦琴X-射线发射

通过氢气放电实验中有无磁场情况下(去掉电子的韧致辐射)X射线谱的比较,指出氢气辉光放电会产生非伦琴X射线发射,X射线能量范围与"电子-离子束缚态及其引发核过程"模型预言的p-e-p～12.5keV、p-e-A+～25keV X射线发射不矛盾.     

太阳耀斑放能机制的讨论——评《太阳高能物理》

本文对《太阳高能物理》所表述的太阳耀斑流行理论作了讨论,给出一种新的太阳耀斑放能机制——"电子—离子束缚态及其引发核过程"模型。并指出太阳耀斑中存在两个独立过程,有～12.5keV(p-e-p～12.5keV)、～25keV(p-e-A ～25keV)、～25keV(d -e-d ～25keV)线发射和(d,d)聚变。对太阳耀斑的一些主要现象作了分析,给出了太阳耀斑中X射线和高能粒子与流行理论不同的产生机制。     

Her X-1是中子星吗?

本文通过对Her X-1的X-ray观测结果和其他中子星X-ray时间变化特征和X-ray谱特征分析,对Her X-1是中子星提出质疑.并根据"电子-离子束缚态及其引发核过程"(简称:电子-离子束缚态)假说,时照太阳耀斑机制,认为Her X-1的辐射可能是它的伴星HZ-Her的耀斑.     

超新星1993J的观测

1993年3月26日西班牙一位天文爱好者F.Garcia用25cm的望远镜在M81(NGC3031)的星系核的西南方向5′处发现了超新星,ST-4的CCD成像系统也记录到这一颗超新星,IAU命名为SN1993J.M81位于大熊座,是旋涡星系(Sb),其距离模数m-M=27.5,即距离d=9.46×10~(19)km.它与M82和NGC3077构成三重星系群.SN1993J是在该星系观测到的第一颗超新星.它是继SN1987A之后观测到最亮的一颗超新星,坐标为:α=9~h51~m19~s.27,δ=69°15′25″7.     

SN1987A超新星和中微子物理

<正> 超新星是恒星在演化过程中从内部发生的大爆发,爆发能量从 10~(48)尔格到10~(52)尔格,今年SN1987A超新星出现是数百年难有的机会。一些物理学家乘机对自己感兴趣的问题进行探测。 今年三月底美国JOHN-HOPKINO大学物理教授C·W·Kim在京访问,三月二十日报告K·Hirata组利用KAMIOKANDE-11探测器探测到SN1987A爆发     

^129Xe^30＋入射Au靶表面的X射线辐射

当不同动能（350-600keV）高电荷态离子129Xe30＋入射Au表面过程中,发出了1.65keV的X射线和靶原子的Mα特征X射线.分析表明：高电荷态离子与Au表面相互作用过程中,Xe离子3d壳层的电子被激发,形成空穴,4f电子偶极跃迁辐射1.65keVM-X射线.同时,靶原子Au的3s电子被激发,退激辐射M-X射线.利用经典过垒模型解释了Xe的M-X射的产额随入射离子的动能增加而减小,靶原子的特征X射线产额随入射离子的动能增加而增加的原因.     

基于能量传递的Pr3+:Ce3+:ZBLAN光纤中上转换激光器的研究

在Pr3+:Ce3+:ZBLAN光纤中,研究了Pr3+的4f5d上转换激发后向Ce3+的5d能级进行能量传递产生激光的可行性.考虑了以1D2为上转换中间能级的最佳泵浦方案,利用相关实验数据建立了粒子数速率方程和传播方程.经过数值计算表明:在此光纤中利用Pr3+向Ce3+的能量传递过程中,能够产生以Ce3+的5d能级为工作能级的激光振荡;最佳光纤长度为0.2m;输出镜的最佳反射率为70%～90%;阈值泵浦功率在20W以上.     

类氖和类钠钨离子LMM双电子复合过程的研究

基于相对论组态相互作用理论方法,系统研究了类氖和类钠钨离子的LMM双电子复合过程(DR).考虑了电子关联效应、Breit相互作用、QED等效应,计算给出了LMM-DR过程相关的W63+,W62+离子单、双激发态的能级和相关的辐射、Auger几率,以及DR过程的强度和截面.基于理论计算,对Tokyo-EBIT实验测得的1.0~5.0keV能区的X射线谱进行了模拟和分析,理论计算很好地模拟并标识出了实验谱中来自W64+和W63+离子的共振峰.     

二步共振激发钙蒸汽产生的250～400nm紫外受激和相干辐射

本文报道二步共振激发钙原子产生250～400nm波段内一系列紫外辐射的研究结果,分析了辐射产生的机制,确认部分辐射由四波混频过程产生,部分辐射是起始于高三重态的受激辐射,并讨论了高三重态的布居机制.     

An asymmetric distribution of positrons in the Galactic disk revealed by gamma-rays

Gamma-ray line radiation at 511 keV is the signature of electron-positron annihilation. Such radiation has been known for 30 years to come from the general direction of the Galactic Centre, but the origin of the positrons has remained a mystery. Stellar nucleosynthesis, accreting compact objects, and even the annihilation of exotic dark-matter particles have all been suggested. Here we report a distinct asymmetry in the 511-keV line emission coming from the inner Galactic disk ( approximately 10-50 degrees from the Galactic Centre). This asymmetry resembles an asymmetry in the distribution of low mass X-ray binaries with strong emission at photon energies >20 keV ('hard' LMXBs), indicating that they may be the dominant origin of the positrons. Although it had long been suspected that electron-positron pair plasmas may exist in X-ray binaries, it was not evident that many of the positrons could escape to lose energy and ultimately annihilate with electrons in the interstellar medium and thus lead to the emission of a narrow 511-keV line. For these models, our result implies that up to a few times 10(41) positrons escape per second from a typical hard LMXB. Positron production at this level from hard LMXBs in the Galactic bulge would reduce (and possibly eliminate) the need for more exotic explanations, such as those involving dark matter.     

MCG-6-30-15的铁Ka线的研究

活动星系核的X射线性质是近几十年X射线天文学研究的一大热点。铁Ka线位于X波段的6-7keY能区,是来自活动星系核中的冷物质的荧光辐射。随着XMM-Newton和Chandra等高性能X射线望远镜投入使用,铁Ka线的研究也更加深入。通常,宽的铁Ka线被认为是研究AGN中心黑洞最好的探针,一个最著名的例子就是MCG-6-30-15。ASCA和XMM-Newton卫星已经对MCG-6-30-15进行了多次观测和研究,发现有明显的宽的铁Ka线存在。研究铁Kn线的轮廓能给出黑洞自旋的一些信息,这些信息对了解黑洞的吸积、演化有重要意义。文章选取XMM-Newton卫星已对MC@6-30-15的一次观测来研究MC@6-30-15铁Ka线性质。     

有挠引力理论对SN1987A中微子两次信号的解释

用有挠引力理论的粒子运动方程探讨了ＳＮ１９８７Ａ中微子的运动，得出中微子可沿两条路径经历不同的时间到达地球的结论，对所观察到的中微子两次信号作出了比较合理的解释。     

Search for hard X-ray emission from the galactic plane

An X-ray survey experiment, consisting of four balloon-borne X-ray telescopes, was flown over Texas last year to search for hard X-ray emission (E(x) > 20 keV) from the Galaxy.     

Rapid X-ray flaring from the direction of the supermassive black hole at the Galactic Centre.

The nuclei of most galaxies are now believed to harbour supermassive black holes. The motions of stars in the central few light years of our Milky Way Galaxy indicate the presence of a dark object with a mass of about 2.6 x 106 solar masses (refs 2, 3). This object is spatially coincident with the compact radio source Sagittarius A* (Sgr A*) at the dynamical centre of the Galaxy, and the radio emission is thought to be powered by the gravitational potential energy released by matter as it accretes onto a supermassive black hole. Sgr A* is, however, much fainter than expected at all wavelengths, especially in X-rays, which has cast some doubt on this model. The first strong evidence for X-ray emission was found only recently. Here we report the discovery of rapid X-ray flaring from the direction of Sgr A*, which, together with the previously reported steady X-ray emission, provides compelling evidence that the emission is coming from the accretion of gas onto a supermassive black hole at the Galactic Centre.     

SN1987a遗留脉冲星的引力辐射

本文讨论了超新星SN 1987a遗留下来的脉冲星的引力辐射。其引力波的无量纲振幅的最大可能量级为10~(-23)。这为引力波的探测提供了一个新的希望。     

The magnetic field of an isolated neutron star from X-ray cyclotron absorption lines

Isolated neutron stars are highly magnetized, fast-rotating objects that form as an end point of stellar evolution. They are directly observable in X-ray emission, because of their high surface temperatures. Features in their X-ray spectra could in principle reveal the presence of atmospheres, or be used to estimate the strength of their magnetic fields through the cyclotron process, as is done for X-ray binaries. Almost all isolated neutron star spectra observed so far appear as featureless thermal continua. The only exception is 1E1207.4-5209 (refs 7-9), where two deep absorption features have been detected, but with insufficient definition to permit unambiguous interpretation. Here we report a long X-ray observation of the same object in which the star's spectrum shows three distinct features, regularly spaced at 0.7, 1.4 and 2.1 keV, plus a fourth feature of lower significance, at 2.8 keV. These features vary in phase with the star's rotation. The logical interpretation is that they are features from resonant cyclotron absorption, which allows us to calculate a magnetic field strength of 8 x 10(10) G, assuming the absorption arises from electrons.     

年青行星状星云NGC7027 HCO^＋谱线发射的一个模型

对在年青行星状星云 NGC7027中新发现的 HCO~+分子离子谱线进行了研究.采用具有不同速度的双壳层膨胀模型,计算了 NGC7027 HCO~+,J=1-0,v=89.2GHz 的谱线发射.将模型结果与观测资料进行比较,导出了双壳层的膨胀速度和半径.发现谱线的理论轮廓与观测轮廓符合甚好.它说明,双壳层的运动学模型对年青行星状星云离子分子谱线的形成可能有重要的作用.     

混凝土硫酸盐腐蚀损伤的声波与声发射变化特征及机理

试验模拟干湿循环作用下混凝土受10%(质量分数)硫酸钠溶液侵蚀的腐蚀环境,测试和分析硫酸盐不同侵蚀时期混凝土单轴压缩试验时波速和声发射的变化特征。采用环境扫描电镜和能谱仪进行微观观测并结合X射线衍射测试手段分析受蚀混凝土的损伤机理。结果表明：受侵蚀60 d和80 d的试件加载初期会有较明显的压密阶段,试件受硫酸盐侵蚀和干湿循环作用愈久,加载中波速急剧下降的突变点愈提前;受蚀40 d以上的试件加载中声发射事件活跃区间较集中,在腐蚀产生的缺陷和薄弱位置容易出现应力集中和能量集中释放,声发射事件数量急剧上升的突变点提前。通过数学模型以声发射累积振铃计数为损伤变量建立损伤模型可以表征混凝土中环境腐蚀、荷载及损伤之间的作用关系。腐蚀阶段钙矾石与石膏的膨胀作用和硫酸钠的结晶压在试件内部形成微破损,受蚀混凝土表现出不同宏观性能。     

Ground-based observation of emission lines from the corona of a red-dwarf star

All 'solar-like' stars are surrounded by coronae, which contain magnetically confined plasma at temperatures above 106 K. (Until now, only the Sun's corona could be observed in the optical-as a shimmering envelope during a total solar eclipse.) As the underlying stellar 'surfaces'-the photospheres-are much cooler, some non-radiative process must be responsible for heating the coronae. The heating mechanism is generally thought to be magnetic in origin, but is not yet understood even for the case of the Sun. Ultraviolet emission lines first led to the discovery of the enormous temperature of the Sun's corona, but thermal emission from the coronae of other stars has hitherto been detectable only from space, at X-ray wavelengths. Here we report the detection of emission from highly ionized iron (Fe XIII at 3,388.1 A) in the corona of the red-dwarf star CN Leonis, using a ground-based telescope. The X-ray flux inferred from our data is consistent with previously measured X-ray fluxes, and the non-thermal line width of 18.4 km s-1 indicates great similarities between solar and stellar coronal heating mechanisms. The accessibility and spectral resolution (45,000) of the ground-based instrument are much better than those of X-ray satellites, so a new window to the study of stellar coronae has been opened.