气球硬X射线探测中方位,仰角的测试电路

本叙述了高空气球探测硬Ｘ射线方位、仰角的测试电路。在气球探测中，方位、仰角的测试是至关重要的一环。是关系到整个探测成功与否的关键。设计中尽可能简单、可靠。方位顺时针、反时针皆顺转自如，其方位角测量范围为０￣３６０°，其精度０．１°；俯仰顺时针、逆时针顺转自如，仰角测量范围０￣９０°，甚至到１２０°也可，其精度为０．１°。     

A Two—Temperature Supernova Fallback Disk Model for Anomalous X—ray Pulsars

We present a case study of the relevance of the radially pulsational instability of a two-temperature accretion disk around a neutron star to anomalous X-ray pulsars (AXPs). Our estimates are based on the approximation that such a neutron star disk with mass in the range of 10^-6-10^-5M⊙ is formed by supernova fallback. We derive several peculiar properties of the accretion disk instability: a narrow interval of X-ray pulse periods; lower X-ray luminosities; a period derivative and an evolution time scale. All these results are in good agreement with the observations of the AXPs.     

地表空气中天然伽玛放射体的测量

本文提出一种估算空气中悬浮放射性核素的附差部分与非附着部分的简易方法，该方法同时采用纤维素与活性炭两种过滤器。利用伽玛射线能谱法系统地检测了近地表空气中一些原生放射性核素的浓度：＾４０Ｋ、＾２２６Ｒａ、＾２１２Ｐｂ、＾２１４Ｐｂ、＾２０３Ｔｌ和＾２１４Ｂｉ，同时还测定了宇宙成因的放射性核素＾７Ｂｅ的浓度。     

两类γ暴的谱形和光变曲线的统计差异的K-S检验

最近的研究表明：短γ射线暴（γ暴）的辐射特性和长γ暴的前两秒的辐射特征相似，这引发了对以前争论的问题，即：这两类暴是否是本质上相同的暴？本文主要对和γ暴谱形和光变曲线有关的两个量的分布进行了K—S检验。分析表明：这两类暴的分布是不同的，这和广为接受的两类γ暴事件产生于不同机制的观点是一致的。     

X Per新发射相的不寻常变化

对ＸＰｅｒ新发射相连续四年的光学光谱和近红外光度监测结果，ＸＰｅｒ近两年的变化不同寻常，主要表现以下两点：（１）尽管它的光学光度Ｖ星等只恢复至失去气壳前的亮度，但Ｈａ发射线等值宽度和近红外，Ｊ，Ｈ和Ｋ光度地超过了历史记录的最大值，分别达到了１６．３４Ａ和５．３＾ｍ，５．３＾ｍ和５．１＾ｍ，表明ＸＰｅｒ新发射相气南的密度和尺度较都大，（２）我们首次观测到ＸＰｅｒ近红外光度和Ｈα发射线等值宽度变化趋势     

用γ射线和α粒子方法测定样品中的钍含量

为测定天然样品中的钍含量，已完成了改进径迹技术的试验。对于钍含量的测量，采用了能量为１８和２０ＭｅＶ的γ射线。对能量范围为６～２３．５ＭｅＶ的γ射线，已获得了对于厚靶的铀，钍元素的裂变碎片径迹密度比ＮＵ／ＮＴＨ。比值为１．７～３．２，其中与最大值对应的γ射线能量为１５ＭｅＶ。在实验误差范围内，标定的ＴＨ标准样和铁锰结核测定的钍含量与知值是一致的。对９．１ＭｅＶ／ｎ的α粒子，已发现径迹密度比ＮＴＨ／     

Can the bump in the composite spectrum of GRB 910503 be an emission line feature of gamma-ray bursts？

Appearing in the composite spectral data of BATSE, EGRET and COMPTEL for GRB 910503, there is a bump at around 1600 keV. We perform a statistical analysis on the spectral data, trying to find out if the bump could be accounted for by a blue-shifted and significantly broadened rest frame line due to the Doppler effect of an expanding fireball surface. We made an F-test and adopted previously proposed criteria. The study reveals that the criteria are well satisfied and the feature can be interpreted as the blue shifted 6.4 keV line. Prom the fit with this line taken into account, we find the Lorentz factor of this source to be P = 116-9+9 (at the 68% confident level,△x2 = 1) and the rest frame spectral peak energy to be E0,p- 2.96-0.18+0.24 keV. Although the existence of the emission line feature requires other independent tests to confirm, the analysis suggests that it is feasible to detect emission line features in the high energy range of GRB spectra when taking into account the Doppler effect of fireball expansion.     

矿物表面分析技术及其应用

本文介绍Ｘ－射线光电子能谱及俄歇电子能谱在矿物表面分析技术中的应用，介绍了某些实例。