适合于印刷品评价与控制的色度仪应满足的条件

本文从印刷工业颜色测量的需要出发,根据色度学理论、人的视觉特性和对印刷过程的分析提出印刷品评价对颜色测量仪的要求。包括对颜色测量理论的选择,对测量几何的要求;对测量光孔和测试色定位的要求;对照明光源和标准观察者类型的选择;对测量值的输出和测量速度等要求。这些内容对色度仪的设计和使用都具有重要意义。     

初动在核爆监测中的应用及分析

核爆炸与地震相比,围绕爆炸源的初动具有更多的向上记录和更高的振幅周期比,初动可以作为核爆与地震的一个识别标志。某些核爆炸的向下记录。或许是由于低信噪比的原因,记录到的是初至波的第二个半周;其余的也许是由于近P波走时曲线的反射波造成。     

Threat level green: Conceding ecology for security in eastern Europe and the former Soviet Union

Following the collapse of the Soviet Union, the predicted scenarios of Central Asian water wars and catastrophic nuclear accidents have failed to materialize. However, the Aral Sea continues to shrink apace, and dangerous Soviet-built nuclear reactors have since proliferated in the former eastern bloc. These seemingly paradoxical outcomes can in part be attributed to the framing of these environmental issues as security matters by leading international regulatory, aid and lending institutions. Integrating these environmental concerns with the realist worldview of security studies systematically emphasized security dimensions at the expense of ecological concerns even amongst organizations distant from traditional defense affairs. This article proposes that international security strategy in this period is one of environmental appeasement defined as the systematic granting of ecologically unfriendly concessions in order to reduce short-term security risks. The article presents evidence that this appeasement strategy generated seemingly impressive results in terms of ameliorating short-term security risks, while actually exacerbating the underlying ecological situation. The article argues that while the foundational environmental risks remain unaddressed, the associated security threats have likewise not been ultimately resolved.     

地铁工程勘察现状与技术研究课题

地铁勘察的特点:一是没有征地的勘察,二是地下系统工程的勘察;我国地铁勘察经历了探索、积累和规范化的历史发展时期,各时期按照可行性研究、初步勘察、详细勘察、施工勘察四个勘察阶段进行工作;根据地铁设计要求和地质条件采取多样化的测试手段,勘察内容全面,技术逐步完善,具有明显的专业特色;今后应结合地铁施工方法和设计要求,研究和总结特殊设计指标的测试技术,解决地铁结构在第四系饱和砂层中的抗震设计问题,加强施工新技术和新方法在不同地质条件下的适应性研究,在安全、快速施工和降低造价等方面不懈努力。     

提高地磁绝对观测数据精度的有效途径

经过长期观察发现用CZM-2型核旋仪(及其同类仪器)进行定点观测读数时,运用分量仪线圈“单向”旋转的方法进行分量观测,再加上做好一些其它辅助措施,能够充分消除人为因素和仪器本身误差所带来的影响,明显提高仪器的观测精度,达到使观测资料更加准确的目的。     

曲线拟合在核探测器信号幅度提取中的应用

研究数字化核探测器输出脉冲信号的幅度提取问题。根据闪烁探测器的电路特性，推导了其脉冲信号理想曲线方程。综合利用三和值法、最小二乘法、试探法等方法，设计了该理想曲线拟合算法。由脉冲信号采样点数据，通过曲线拟合，计算出曲线的极大值，该值即为闪烁探测器输出脉冲信号的幅度。正反演数据结果对比表明，采用曲线拟合算法提取闪烁探测器输出脉冲信号幅度，其方案可行，计算结果更准确。相较于数字滤波和数字脉冲成形方法提取核探测器输出脉冲幅度，该算法更简单，对仪器的硬件处理速度要求更低。该方法开辟了核探测器脉冲幅度提取的新途径。     

Double detonations at the core–envelope boundary in Type Ia supernovae

An off-centre detonation propagating near the interface between a C–O core and a He envelope in a Type Ia supernova explosion is modelled as a steady two-dimensional similarity solution at a plane interface. We assume that in both regions the energy release occurs in an infinitely thin detonation, which produces material in nuclear statistical equilibrium (NSE) in He and in nuclear statistical quasi-equilibrium in C–O. An α-network is then used to determine the effect of the associated rarefaction wave in the C–O on the final abundance of intermediate elements. We find that, although there is a significant effect, the rarefaction is not strong enough to quench the reactions and prevent the C–O from burning to NSE.     

秩亏自由网平差的一种新解法

提出秩亏自由网平差的一种新解法,只亲知道误差方程系数阵中ｔ０个线性无关的列向量,就能很快地得到最小二乘最小范数解,实际计算表明,这种新解法是简单有效的。     

Heavy-element abundances in seven SC stars and several related stars

We employ spectra of resolution 20–35000 of seven SC stars, four S stars, two Ba stars and two K–M stars to derive abundances of a variety of elements from Sr to Eu relative to iron. Special attention is paid to Rb and Tc, and to the ratio of the heavy s-process species to the light s-process elements. Abundances are derived in LTE, both by using model atmospheres in which the carbon and oxygen abundances are nearly equal and by using curves of growth. Spectrum synthesis is used for critical lines such as the 5924-Å line of Tc and the 7800-Å line of Rb. For most of the heavy-element stars the enhancement of the s-process elements is about a factor of 10. The ratio of the heavy to light s-process species is not far from solar, except for RR Her for which the same ratio is +0.45 dex. For Tc the blending by other lines is severe. While we have probably detected the 5924-Å line, we can only present abundances in the less-than-or-equal-to category. For Rb, whose abundance is sensitive to the ⁸⁵Rb/⁸⁷Rb ratio and hence to the neutron density during s-process production, we find a considerable range of abundances, indicating a neutron density from 10⁶ to ≳10⁸ cm⁻³ for the SC stars. For the four S stars the range is from 10⁷ to ≳10⁸ cm⁻³. Recent calculations by Gallino et al. show that neutron densities near 10⁷ cm⁻³ favour the ¹³C source for neutrons, while densities greater than 10⁸ cm⁻³ may be associated with neutrons from the ²²Ne source.