Pulsar Wind Nebulae in Egret Error Boxes

A remarkable number of pulsar wind nebulae (PWN) are coincident with EGRET γ-ray sources. X-ray and radio imaging studies of unidentified EGRET sources have resulted in the discovery of at least six new pulsar wind nebulae (PWN). Stationary PWN (SPWN) appear to be associated with steady EGRET sources with hard spectra, typical for γ-ray pulsars. Their toroidal morphologies can help determine the geometry of the pulsar which is useful for constraining models of pulsed γ-ray emission. Rapidly moving PWN (RPWN) with more cometary morphologies seem to be associated with variable EGRET sources in regions where the ambient medium is dense compared to what is typical for the ISM.     

Parameters of the intense X-ray and gamma-ray radiation from the solar flare of May 20, 2002, as observed from the Coronas-F spacecraft

We consider temporal, spectral, and polarization parameters of the hard X-ray and gamma-ray radiation observed during the solar flare of May 20, 2002, in the course of experiments with the SONG and SPR-N instruments onboard the Coronas-F spacecraft. This flare is one of the most intense gamma-ray events among all of the bursts of solar hard electromagnetic radiation detected since the beginning of the Coronas-F operation (since July 31, 2001) and one of the few gamma-ray events observed during solar cycle 23. A simultaneous analysis of the Coronas-F and GOES data on solar thermal X-ray radiation suggests that, apart from heating due to currents of matter in the the flare region, impulsive heating due to the injection of energetic electrons took place during the near-limb flare S21E65 of May 20, 2002. These electrons produced intense hard X-ray and gamma-ray radiation. The spectrum of this radiation extends up to energies ≥7 MeV. Intense gamma-ray lines are virtually unobservable against the background of the nonthermal continuum. The polarization of the hard X-ray (20–100 keV) radiation was estimated to be ≤15–20%. No significant increase in the flux of energetic protons from the flare under consideration was found. At the same time, according to ACE data, the fluxes of energetic electrons in interplanetary space increased shortly (～25 min) after the flare.     

Future goals for γ-ray spectroscopy

Gamma-ray lines are the fingerprints of nuclear transitions, carrying the memory of high energy processes in the universe. Setting out from what is presently known about line emission in gamma-ray astronomy, requirements for future telescopes are outlined. The inventory of observed line features shows that sources with a wide range of angular and spectral extent have to be handled: the scientific objectives for gamma-ray spectroscopy are spanning from compact objects as broad class annihilators, over longlived galactic radioisotopes with hotspots in the degree-range to the extremely extended galactic disk and bulge emission of the narrow e^– e⁺ line.The instrumental categories which can be identified in the energy range of nuclear astrophysics have their origins in the different concepts of light itself: geometrical optics is the base of modulating aperture systems-these methods will continue to yield adequate performances in the near future. Beyond this, focusing telescopes and Compton telescopes, based on wave- and quantum- optics respectively, may be capable to further push the limits of resolution and sensitivity.     

Airborne gamma-ray spectrometry to quantify chemical erosion processes

Airborne gamma-ray spectrometry data (uranium, potassium and thorium contents) reveal geochemical heterogeneities within the monolithological Hyrôme watershed (ca. 150 km²) in the Armorican massif (western France). Our observations and computations provide important constraints on the spatial distribution and the associated magnitudes of chemical erosion processes at the scale of a small watershed. Two distinct, partially preserved, weathering profiles exhibit a strong correlation between regolith evolution and airborne-derived K/Th ratios, suggesting that the variability is linked to supergene processes. Using both airborne data and laboratory measurements on rock samples, the total net export of potassium has been estimated at 422 ± 50 kg/m² and the chemical weathering rate of potassium at 17 ± 2 kg/km²/a.     

湖相致密储层有利层段的沉积与湖平面变化的耦合关系及其控制因素：以柴西尕斯地区上干柴沟组下段为例

探讨有利层段的沉积与湖平面变化之间的关系,可以对湖相致密储层的勘探开发部署提供一定参考。以柴达木盆地西部尕斯地区上干柴沟组下段为例,利用自然伽马（GR）曲线资料,进行Fischer图解和铀含量（U）－有机碳（TOC）回归拟合法,重建渐新世沉积时期湖平面变化过程,结合磁化率资料,讨论了湖平面变化的气候控制作用。结果表明：（1）尕斯地区上干柴沟组下段泥质含量和TOC含量变化趋势一致,均反映其在沉积过程中经历了两次湖退和湖进过程,有利于烃源岩和储层的形成;（2）湖平面上升期形成的高水位沉积体系,对应于致密砂岩类储层中优质烃源岩的富集层段,能有效形成源－储共生配置;（3）渐新世湖平面变化受西风条件下的气候的控制,西风带来的水汽,形成相对湿润的气候条件,引起湖平面的上升,有利于烃源岩的形成,且与有利层段的沉积呈现耦合关系。

     

基于单能窄束伽马射线算法计算高分辨率屏蔽自然伽马探测器的三维测井响应

本文应用单能窄束伽马射线理论建立高分辨率屏蔽自然伽马探测器三维测井响应的数值模拟算法.首先利用单能窄束原理,用稳态扩散方程描述伽马光子密度的空间分布,根据扩散方程基本解、放射源空间分布、探测器位置和屏蔽情况,将屏蔽探测器上的总伽马通量表示成放射性地层中的有效探测区域上的体积分和晶体表面上有效接收面的面积分形式.并根据伽马射线传播路径和探测器屏蔽情况,给出有效探测区域的解析表达式,通过数值积分法计算任意复杂情况下探测器上的自然伽马通量,获得伽马测井响应的3D数值模拟算法.并通过数值模拟结果与模型井数据的对比验证了该算法的有效性.最后通过3D数值模拟算法系统研究考察晶体形状（圆柱形晶体、方形晶体）、晶体长度、仪器在井轴中的位置（居中屏蔽探测器、贴井壁屏蔽探测器）、以及测速等不同情况下自然伽马测井响应,设计出新型高分辨率自然伽马测井仪器.     

东营凹陷牛38井沙三段高分辨率旋回地层研究

自然伽玛测井资料取自山东省东营市胜利油田的牛38井。该井的沙河街组划分为四个段,其中沙三段依据含艾氏鱼群组合的鲱科化石和沉积物旋回堆积速率(AR)等研究,可与北美始新统绿河组进行对比。根据上世纪90年代沙三段古地磁研究结果,井深3263m处C18n.1n/C18n.1r界线调整为38.975MaBP。通过频谱分析和数字滤波计算,得出了沙三段几个界线的年龄值,其中,在沙三下、中亚段界线算出的36.9MaBP,岁差旋回幅度有明显变化,这一变化与Palike(Palikeetal.,2001)在ODP71线1052孔中发现的类似图像(36.7Ma)可比较。     

Swift时代伽马暴的观测及研究进展

Swift卫星从2004年11月20日升空开始运转到现在已有2年多时间.到目前为止,它-共观测到了200多个伽马暴及其余辉现象.由于Swift观测到了早期X射线余辉、短暴余辉和高红移伽马暴等新的重要现象,伽马暴研究进入了新的时代.该文首先对伽马暴的研究历史做简短回顾,然后简要介绍伽马暴的物理图像和Swift卫星的构成及特点,最后全面评述Swift的观测成就及由此引起的理论挑战.     

Occurrence of thorite and radioactive zircon in syenite pegmatite,North of Ashwaraopet,Khammam district,Andhra Pradesh,India

This paper reports the occurrence of thorite and confirms the earlier find of radioactive zircon by Subbarao, Murali and others from syenite pegmatite in the Vinayakapuram-Kunavaram alkaline belt in the Khammam district of Andhra Pradesh, India. Thorite has also been found as residual concentrations in soil overlying the pegmatite.     

顺便伽玛测量在水化普查中的找铀效果

在铀矿普查中,伽玛测量具有经济、快速、轻便、连续测量的特点。在水化普查中作顺便伽玛测量,投资少、收效快,并可直接发现供详查揭露的矿化点。在生产布置上与水化测量相互适应。通过一遍工作之后,可取得2套各具特点的资料。在资料解释及运用上,二者可互为补充。对无水地段,水化测量为空白区,可用伽玛测量补其不足。伽玛测量可为水化异常解释提供资料,水化异常的规模及浓度的高低又是推测深部矿化情况的依据。从统计结果证实,比例尺为上1:2.5万的顺便伽玛测量与1:1万的正规伽玛测量比较,发现异常机率可达60％。可见将顺便伽玛测量资料在测量精度上降一级使用,是可以满足精度要求的。