塔里木盆地奥陶系生物礁露头的地球物理特征

奥陶系生物礁为塔里木盆地重要的储集层,明确露头上生物礁的内部结构及发育规模,探索露头和井下生物礁对比研究的新手段有重要意义。应用探地雷达及自然伽马能谱仪对塔里木盆地巴楚达吾孜塔格奥陶系露头进行了探测。研究表明,探地雷达剖面上多数生物礁为扁平透镜状或层状,这与露头上观察的结果有所差别;高分辨率雷达剖面揭示出较出露生物礁发育程度更大、个体更小的疙瘩状礁体或礁团块;礁体内部的分层性及礁体内部水道充填体的斜层理在雷达剖面上反映明显,雷达分辨率可达到分米级别。礁灰岩的自然伽马值高于亮晶砂、砾屑灰岩,而低于泥晶灰岩、棘屑灰岩、泥晶生屑灰岩、泥灰岩的放射性。生物礁在自然伽马曲线上表现为漏斗形、钟形或箱形;自然伽马曲线也反映出礁体内部的分层性。露头和轮南井下奥陶系生物礁的自然伽马放射性特征有一定的相似性,这为露头和井下生物礁的对比研究提供了有力的辅助手段.     

伽马能谱测量在陆地伽马空气吸收剂量率评价中的应用

2002～200年,国内首次采用就地伽马能谱测量方法在广东珠海市进行了面积性测量,并用该方法定量解释求得的钾、铀、钍含量用Beck公式估算了地表1 m高处的吸收剂量率,同时用塑料闪烁体X-γ吸收剂量率仪在相同测点做了比对测量.2种方法对比结果(514个测点)显示很好的一致性,珠海市区实测吸收剂量率和伽马能谱估算吸收剂量率平均值分别为(145.07±26.5) nGy/h和(162.10±1.51) nGy/h,计算结果与实测结果的相对误差为11.74%.     

Aeromagnetic And Aeroradiometric Response To Hydrothermal Alteration

In Precambrian terrains all regional and most localintensive magnetic anomalies areproduced by magnetite. Monoclinic pyrrhotite isresponsible for some local, but oftenintensive, magnetic anomaly patterns. Both magnetiteand pyrrhotite are affected byhydrothermal alteration processes in various ways,resulting in changes either inabundance or in grain fabric. These changes arerecorded in the magnetic properties ofthe altered rock units and reflected in theiraeromagnetic signatures. Hydrothermalalteration in deformed bedrock zones is commonlycontrolled by structural or tectonicfeatures. Regional high-resolution aerogeophysicalsurveys can be utilized, in bothregional and detailed investigations, to map theoverall geological and tectonic settingor to estimate local changes in magnetic mineralogyand the relative abundance ofradionuclides.Magnetite is most commonly destroyed in alterationprocesses, such as biotitization,carbonation, sulfidization and silicification. Theprogressive destruction of magnetitebegins at grain margins and results first in broken and cracked grain texture and smallergrain size, then progresses to total disappearanceof magnetite. Alteration in magnetite-bearing rock units may be recognized by decreasedmagnetic intensity and by thebroken, disrupted magnetic pattern. The abundance ofmonoclinic pyrrhotite isenhanced by reducing hydrothermal fluids, and typicalcrystal anisotropy is developeddue to tectonic stress.The relative contents of radioelements are changedin the same hydrothermal processesand partly for the same reasons as the ferrimagneticminerals. Potassic alteration oftenresults in elevated K radiation particularly formafic rocks, and then anomalous K/Thratios along local shear or fracture zones may beindicative of gold-bearingmineralization. On the other hand, high U/Th ratioswithin metasedimentary units maypoint out prospects for sulphidization. Althoughvariation of U/Th ratios largely reflectsthe environmental conditions during primarydiagenesis or a later deformational phase,mainly the decrease in Th radiation close tosulphide mineralization seems to beresponsible for the elevated U/Th ratios.     

Drive-Control System for the TACTIC Gamma-Ray Telescope

A PC-based drive-control system has been developed for the altitude-azimuth mounted TACTIC -ray telescope to control the speed and direction of motion of its 2-axes. Details of various hardware components chosen for the telescope, including hybrid-stepper motor, 16-bit absolute encoder and CAMAC-based programmable stepper motor controller, are discussed in this paper. The telescope-control strategy, based on the position-loop with a proportional type control for the source-seek mode and the on/off type control for the tracking mode, is explained in detail. Some important performance features of the telescope, including its blind-spot size, drive-system backlash and encoder-error compensation, are also presented. The drive system has been extensively field-tested and has been operating satisfactorily during observation campaigns carried out since March 1997 with the TACTIC Imaging Element. A tracking accuracy of ±3 arc-minutes has been achieved. A test report of its performance, with regard to its tracking accuracy on the basis of successful detection of TeV -rays from the active galaxy Markarian 501 in April–May 1997, is also presented.     

Discovery of an optical afterglow from the cosmic GRB 920925C

A systematic study of the archival images for the error boxes of cosmic gamma-ray bursts (GRBs) obtained at the Palomar (USA) and Siding Spring (Australia) Observatories during the DSS allsky survey has revealed an optical transient with a magnitude of 17.8 within the error circle of the bright event GRB 920925C on the plate taken 6 h after the burst. The position of the object falls within the IPN error box for the burst. Analysis of the event properties suggests that the detected transient is most likely the optical afterglow from GRB 920925C. This event occurred 4.5 yr before GRB 970228, which has been considered to be the first optically identified GRB up until now.     

Discovery of an optical flare from GRB 060926 by the MASTER robotic telescope: Possible formation of a marginally rotating black hole

The MASTER robotic telescope has obtained the first optical images of GRB 060926. We have discovered an optical flare from GRB 060926, a recurrent brightening that closely follows its behavior in the X-ray range. We have determined the spectral slope for GRB 060926 from the X-ray to optical range in the first minutes. Based on the spinar model, we show that the parameters of the optical and X-ray flares suggest that the gamma-ray burst resulted from the core collapse of a 7M _⊙ star with an initial effective Kerr parameter of 7.6 and an initial magnetic-to-gravitational energy ratio of 10^?4.     

同步辐射和费米伽马暴光谱的一致性检验

定义了一个新的量,曲率宽度,去检查同步模型与伽玛射线暴(GRB)光谱的一致性.此量用于测量GRB中辐射能谱(νFν,ν和Fν分别是频率和随频率变化的能量流量)峰值处的光谱拐折锐度.然后使用它检查了理论同步模型与观测到的GRB光谱之间的一致性.首先计算几种典型的同步模型的曲率宽度,包括单能、单幂律和拐折幂律电子同步模型.其次从Fermi/GBM (Gamma-ray Burst Monitor)长GRB时间分辨光谱目录中选择包含1198个光谱的GRB样本,将光谱与常用的经验模型拟合,并计算最佳拟合模型的光谱曲率宽度.通过比较两个曲率宽度,发现大多数样本与同步模型不一致,因为同步模型的光谱拐折比数据的光谱拐折更加平滑.结果表明同步模型很难适合大多数观测到的GRB光谱.此外,在暴脉冲中发现光子流量和曲率宽度之间存在强的反相关性,这表明流量越高,光谱拐折越尖锐,或者与同步模型的偏差就越大.     

Observations of soft gamma-ray or hard X-ray bursts in the GRIF experiment on the <Emphasis Type="Italic">Mir</Emphasis> orbiting station

During the GRIF experiment onboard the Mir orbiting station, the sky was monitored with a PX-2 wide-field (～1 sr) scintillation X-ray spectrometer to detect bursts in the photon energy range 10–300 keV. Because of the comprehensive instrumentation, which, apart from the X-ray and gamma-ray instruments, also included charged-particle detectors, the imitations of astrophysical bursts by magnetospheric electron precipitations and strongly ionizing nuclei were effectively filtered out. It was also possible to separate solar and atmospheric events. Several tens of bursts interpreted as being astrophysical were detected in the experiment at sensitivity levels S～10^?7 erg cm^?2 (for bursts whose spectra were characterized by effective temperatures kT～100 keV) and S～3×10^?8 erg cm^?2 (for bursts with kT～25 keV). Some of the soft gamma-ray or hard X-ray bursts with kT～10–50 keV were identified with the bursting pulsar GRO J1744-28. Our estimate of the detection rate for cosmological soft gamma-ray or hard X-ray bursts from the entire sky suggests that the distributions of long-duration (>1 s) gamma-ray bursts (GRBs) in characteristic energy kT and duration are inconsistent with the steady-state cosmological model in which the evolution of burst sources is disregarded. Based on GRIF and BATSE/CGRO data, we conclude that most of the GRB sources originate at redshifts 1<z<5.     

γ射线暴谱硬度比的时间演化特征

采用小波分析方法对康普顿γ射线天文台(CGRO)上的BATSE仪器观测到的γ暴光变曲线数据进行去噪处理,并提出时间分辨的谱硬度比定义,用包含有599个暴的样本研究谱硬度比随时间的演化规律,结果表明:(1)样本中77%暴的谱硬度比随时间按"硬到软"规律演化,而23%暴谱硬度比随时间按"软到硬"规律演化,尤其是3%暴在整个暴中呈现单调的"软到硬"趋势。(2)平均谱硬度比随时间单调地以"硬到软"规律演化。(3)持续时间不同的暴,其谱硬度比演化曲线有较大的差异,其中"硬到软"演化趋势最显著的是持续时间在23～35s之间的那些暴;持续时间在1～10s的暴的演化特征跟其它组差异最显著,呈现比较明显的"软到硬"演化规律;持续时间在35～53s之间的暴平均谱硬度比几乎没有随时间演化。(4)不同辐射强度的暴平均谱硬度比的演化特征不同,随着峰值流量的增大,谱硬度比演化由"硬-软-硬"逐渐转变为"软-硬-软":峰值流量越大,"软-硬-软"的趋势越显著,而峰值流量越小,其峰值流量"硬-软-硬"的趋势越显著。我们对这些结果进行了简单的讨论。     

IGR J16318-4848: An X-ray source in a dense envelope?

We analyze in detail the ASCA observations of the hard X-ray source IGR J16318-4848, which was recently discovered by the INTEGRAL observatory (Courvoisier et al. 2003). The source has an anomalously hard spectrum in the energy range 0.5–10 keV and is virtually undetectable below 4 keV because of strong photoabsorption (n _H L>4×10²³ cm^?2). The Kα line of neutral or weakly ionized iron with an equivalent width of ～2.5 keV dominates in the energy range 4–10 keV. There is also evidence for the presence of a second line at energy ～7 keV. Our analysis of archival observational data for the infrared counterpart of IGR J16318-4848 that was discovered by Foschini et al. (2003) revealed the source in the wavelength range 1–15 µm. Available data suggest that the object can be an X-ray binary system surrounded by a dense envelope. The source may be a high-mass X-ray binary similar to GX 301-2. We believe that IGR J16318-4848 can be the first representative of a hitherto unknown population of strongly absorbed Galactic X-ray sources that could not be detected by previous X-ray observatories.