A search for ultra-high energy counterparts to gamma-ray bursts

A small air shower array operating over many years has been used to search for ultra-high energy (UHE) gamma radiation ( 50 TeV) associated with gamma-ray bursts (GRBs) detected by the BATSE instrument on the Compton Gamma-Ray Observatory (CGRO). Upper limits for a one minute interval after each burst are presented for seven GRBs located with zenith angles < 20°. A 4.3 excess over background was observed between 10 and 20 minutes following the onset of a GRB on 11 May 1991. The confidence level that this is due to a real effect and not a background fluctuation is 99.8%. If this effect is real then cosmological models are excluded for this burst because of absorption of UHE gamma rays by the intergalactic radiation fields.     

Room temperature solid-state detectors for Gamma ray burst spectroscopy

We have evaluated several solid state detectors which offer excellent energy resolution at room temperature for soft X-rays. For soft X-rays (< 1 keV to 20 keV), silicon P-intrinsic-N (PIN) and avalanche-mode photodiodes (APD's) have been studied. Using commercially available charge sensitive pre-amplifiers, these photodiodes provide 1 keV resolution without cooling. Their detection efficiencies are limited to about 20 keV and 15 keV, respectively. To overcome this constraint, we have studied thick (1.5 mm) PIN detectors made by Micron Semiconductor Ltd., U.K., as well as compound semiconducting materials with high Z constituents such as CZT and PbI₂. PbI₂ allows high detection efficiencies of photons up to 100 keV with detectors 100–300 microns thick. These new detectors offer the capability to study the low-energy spectral evolution of Gamma ray bursts (GRBs). A matrix of these detectors could be used as an image plane detector with moderate spatial resolution for imaging.     

A GRB model satisfying stringent observational constraints

The temporal behavior of GRBs is quantified using a power spectrum analysis. The power spectrum of great variety of GRBs is well represented by the simple ^–2 behavior. We then study a cosmological GRB model in which relativistic flows interact with dense radiation fields. This mechanism in the densest stellar regions known to exist, surprisingly yields the correct temporal behavior. Other characteristics are also reproduced, including the duration bimodality and the hardness-duration distribution.     

Coalescing neutron stars as gamma ray bursters?

We investigate the dynamics and evolution of coalescing neutron stars. The three-dimensional Newtonian equations of hydrodynamics are integrated by the Piecewise Parabolic Method on an equidistant Cartesian grid. The code is purely Newtonian, but does include the emission of gravitational waves and their back-reaction. The properties of neutron star matter are described by the equation of state of Lattimer and Swesty (1991). Energy loss by all types of neutrinos and changes of the electron fraction due to the emission of electron neutrinos and antineutrinos are taken into account by an elaborate neutrino leakage scheme. We simulate the coalescence of two identical, cool neutron stars with a baryonic mass of 1.6M and a radius of 15 km and with an initial center-to-center distance of 42 km. The initial distributions of density and electron concentration are given from a model of a cold neutron star in hydrostatic equilibrium. We investigate three cases which differ by the initial velocity distribution in the neutron stars. The orbit decays due to gravitational-wave emission and after one revolution the stars are so close that dynamical instability sets in. Within 1 ms the neutron stars merge into a rapidly spinning (P 1 ms), high-density body ( 10¹⁴ g/cm³) with a surrounding thick disk of material with densities 10¹⁰ – 10¹² g/cm³ and orbital velocities of 0.3-0.5 c. The peak emission of gravitational waves has a maximum luminosity of a few times 10⁵⁵ erg/s and is reached for about 1 ms. The amplitudes of the gravitational waves are close to 3 10^–23 at a distance of 1 Gpc and the typical frequency is near the dynamical value of the orbital motion of the merging neutron stars of 2 KHz. In a post-processing step, the rate of neutrino-antineutrino annihilation is calculated from the neutrino luminosities generated during the hydrodynamical simulations. We find the integral annihilation rate to be a few 10⁵⁰ erg/s during the phase of strongest neutrino emission, which is too small to generate the observed bursts considering the fact that the merged object of about 3M will most likely collapse to a black hole within milliseconds.     

斯通利波和渗透率的关系分析

理论和实际资料证明,在渗透性地层,低频斯通利波出现的频散和能量衰减与地层渗透率有关,因此可利用斯通利波的传播速度和能量衰减等特性来估算地层渗透率。斯通利波的能量和渗透率负相关。因为斯通利波能量代表了斯通利波的有关信息,因此可以认定斯通利波和渗透率负相关。     

一种基于核学习的储集层渗透率预测新方法

基于核学习的支持向量机,是一种采用结构风险最小化原则代替传统经验风险最小化原则的新型统计学习方法,具有完备的理论基础。这里提出了核学习技术在储集层非均质特性描述中渗透率参数预测的新用途。在复杂地层中,基于支持向量机的智能和自适应模式识别能力而建立了常规测井多参数信息输入的渗透率预测模型,然后对实际油田储集层渗透率进行了预测。与常规线性回归模型预测结果相对比,所提出的方法更易于使用,很少受不确定因素的影响,并具有较强的信息整合能力以及更高的预测准确性和可信度。     

层序的测井、地震响应特征研究

在层序地层学研究中,关键是层序划分和对比。而层序划分、对比的关键是层序识别。层序的识别包括层序界面(层序的底界面、初始海泛面和最大海泛面)的识别和构成层序的体系域识别。这里,在众多前人研究成果的基础上,详细研究了层序的测井、地震响应特征,即层序界面和体系域在测井曲线上和地震剖面上的特征。其中,层序底界面在测井上表现为突变的钟型、箱型或侧积式曲线的底界;在地震剖面上表现为剥蚀、顶超、上超、下超;而体系域在测井曲线上的响应为:低水位体系域的海底扇以漏斗形中、高幅的前积式,或钟型中、低幅的后积式模式为特征,陆坡扇成钟型、正向齿形,自下而上幅度由中高幅→低幅,即具后积式测井模式,低水位楔的测井曲线表现为旋回性进积模式特征,其特征表现为锯齿状箱型。海侵体系域的测井曲线呈现向上变细、变深序列,并表现为钟型、正向齿形或齿化状,幅度由高幅变化为低幅,包络线具后积式特征。高水位体系域相应的测井曲线呈现中幅箱形或桶形,不同体系域在地震剖面上的响应特征明显不同。     

HD-4002型综合测井仪

HD 4002型综合测井仪是核工业北京地质研究院于1998年开始研制的, 其目标是为铀矿地质系统提供适合砂岩型铀矿勘查的轻便型数字测井仪, 满足测井生产的需要。该仪器于2001 年3月通过部级鉴定, 2002至2003年投入海拉尔盆地铀矿勘查测井试生产。本文介绍了仪器的用途、功能及特点、性能指标, 简要说明了各部分的工作原理。     

磁铁石英岩型铁矿岩芯光谱编录研究

 对河北省昌黎县闫庄铁矿床的磁铁石英岩型铁矿石261件样品进行了光谱反射率测量，并与其铁含量进行了相关关系研究，目 的是对钻孔岩芯编录的新方法即高光谱岩芯编录在此类矿床中的可行性进行分析。研究结果表明，铁矿石反射率较低，一般为5%~20% ，铁离子的吸收峰主要表现在400~1 100 nm范围内，铁矿石中铁含量与850~900 nm的反射率均值呈现显著指数负相关关系，为高光谱 岩芯编录在此类矿床中的可行性提供了理论依据和技术途径。