The X-ray spectrum of Cyg X-2

The spectra of disc accreting neutron stars generally show complex curvature, and individual components from the disc, boundary layer and neutron star surface cannot be uniquely identified. Here we show that much of the confusion over the spectral form derives from inadequate approximations for Comptonization and for the iron line. There is an intrinsic low-energy cut-off in Comptonized spectra at the seed photon energy. It is very important to model this correctly in neutron star systems as these have expected seed photon temperatures (from either the neutron star surface, inner disc or self-absorbed cyclotron) of ≈1 keV, clearly within the observed X-ray energy band. There is also reflected continuum emission which must accompany the observed iron line, which distorts the higher energy spectrum. We illustrate these points by a reanalysis of the Ginga spectra of Cyg X-2 at all points along its Z track, and show that the spectrum can be well fitted by models in which the low-energy spectrum is dominated by the disc, while the higher energy spectrum is dominated by Comptonized emission from the boundary layer, together with its reflected spectrum from a relativistically smeared, ionized disc.     

Extended dust shells around carbon stars resolved by “HIRAS”

We have examined forty-two carbon stars which show excess emission at 60 and/or 100µm by applying maximum-entropy image reconstruction techniques to the IRAS 60µm survey data. Thirteen stars are found to be extended in the reconstructed images. Four of them show a detached ring centered on the stellar position. In particular, U Ant may have a double detached dust shell. The implications of our results are discussed concerning the variation of mass loss on the AGB evolution.     

Venus upper atmospheric CO, temperature, and winds across the afternoon/evening terminator from June 2007 JCMT sub-millimeter line observations

The Venus mesosphere constitutes a highly variable transition region between the zonal rotation of the lower atmosphere and the diurnal circulation of the upper atmosphere. It further serves as the primary photochemical region of the Venus atmosphere. We obtained James Clerk Maxwell Telescope (JCMT, Mauna Kea Hawaii) sub-millimeter line observations of mesospheric ¹²CO and ¹³CO during coordinated space (MESSENGER and Venus Express) and ground-based observations of Venus in June of 2007. Such CO spectra line measurements support temperature, CO mixing ratio, and wind retrievals over the 80-110 km altitude range, encompassing the upper mesosphere and lower thermosphere of Venus. Five-point beam integrations were obtained across the observed Venus disk, allowing distinction of afternoon (noon to 6 p.m.) versus evening (6 p.m. to midnight) local times and northern (0-60N) versus southern (0-60S) latitudes. Distinctive diurnal variations (noon to midnight) are retrieved for both temperatures above 95 km and CO mixing ratios above 85 km altitudes. Separate CO line maps obtained on (UT) June 2, 3, 6, and 11 indicate moderate daily variability in afternoon and evening CO mixing ratios (20-50%) and temperatures (5-10 K). Average Venus mesospheric temperatures over this period were 10 K warmer than returned from 1978 to 1979 Pioneer Venus or 2000-01 sub-millimeter measurements, without evidence for the very large temperature inversions indicated by Venus Express SPICAV measurements at 90-100 km altitudes (Bertaux, J.L., Vandaele, A.-C., Korablev, O., Villard, E., Fedorova, A., Fussen, D., Quémerais, E., Belyaev, D., Mahieux, A., Montmessin, F., Muller, C., Neefs, E., Nevejans, D., Wilquet, V., Dubois, J.P. Hauchecorne, A., Stepanov, A., Vinogradov, I., Rodin, A., Bertaux, J.-L., Nevejans, D., Korablev, O., Montmessin, F., Vandaele, A.-C., Fedorova, A., Cabane, M., Chassefière, E., Chaufray, J.Y., Dimarellis, E., Dubois, J.P., Hauchecorne, A., Leblanc, F., Lefèvre, F., Rannou, P., Quémerais, E., Villard, E., Fussen, D., Muller, C., Neefs, E., Van Ransbeeck, E., Wilquet, V., Rodin, A., Stepanov, A., Vinogradov, I., Zasova, L., Forget, F., Lebonnois, S., Titov, D., Rafkin, S., Durry, G., Gérard, J.C., Sandel, B., 2007. A warm layer in Venus’ cryosphere and high-altitude measurements of HF, HCl, H₂O and HDO. Nature 450, 646-649). Measured Doppler shifts associated with June 2 and 11 ¹²CO line center absorptions indicate nearly supersonic (200 m/s, Mach 1) afternoon-to-evening (retrograde) circulation; composed of additive subsolar-to-antisolar (SSAS) and zonal retrograde wind components, which are not separable due to the particular observational geometry.     

The brightness of the galactic radio loops at 1420 MHz: Some indications for the existence of Loops V and VI

In this article we use 1420 MHz data to demonstrate the likely reality of Galactic radio Loops V and VI. We further estimate distances and spectral indices for both these and the four main radio loops. In the cases of Loops I–IV, radio spectral indices are calculated from the mean brightnesses at 1420 and 820/404 MHz. The spectral indices of Loops V and VI are obtained from T –T plots between 1420 and 408 MHz. Using the supernova remnant (SNR) hypothesis for the origin of radio loops, distances are calculated from the surface brightnesses and the angular diameters at 1420 MHz. We also study how results for brightnesses and distances of radio loops agree with current theories of SNR evolution. For this purpose, the ambient density and initial explosion energy of the loops are discussed. We also discuss applications of different Σ–D relations. The results obtained confirm a non‐thermal origin and nearby locations for the Galactic radio loops. Therefore, we have indications that they are very old SNRs that evolve in low ambient densities, with high initial explosion energies. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

龙口的海风及其影响

本文运用龙口气象站近５年自记风资料及实测探空资料，分析了龙口海风的生消规律、海风强度、空间结构及海风生成后对温、湿度的影响。同时为分析海风环流对大气污染物的影响。本文提出了一个简单地计算热内边界层的方法。     

土热传导系数及模型的研究现状和展望

近年来,随着全球能源消耗的增加,对新能源的开发和利用日益重要。地热资源作为一种清洁环保的新能源已经开始引起广泛的关注,对岩土材料的热性质研究也逐渐受到国内外学者的重视。土的热性质包括热传导系数、热扩散系数和比热容。其中,热传导系数作为其中最重要的性质,它不仅决定了热量在土体中的传播速度和土体温度场的分布,同时也是各种地热泵、能量桩等建筑热工结构设计中需要考虑的主要参数之一。首先介绍了土热传导系数的工程背景和研究意义,描述了土中的热量传播方式和类型,阐述了热传导系数的概念,并分析了土热传导系数的各种影响因素（含水率、密度、矿物成分、温度等）。在此基础上,总结了目前国内外土热传导系数模型的研究现状,并对各个模型的优缺点进行了简要的分析和评价。最后,提出了对土传导系数及模型研究的建议和展望。     

基于Clementine热红外数据的Apollo17登月点区域氧化钙含量反演

为了研究利用Clementine热红外数据反演月球表面岩石的氧化钙(Ca O)含量,论文选取了两景覆盖Apollo17登月点的Clementine热红外影像,将其覆盖的区域选为研究区。利用月球表面温度物理模型模拟月表温度,结合普朗克函数,完成发射率反演。在此基础上,对LPI中35个除Apollo17登月计划外所采集的样品Ca O含量与其热红外发射率特征做回归统计分析,发现存在很好的线性关系(R2=0.661)。由此,基于Clementine热红外发射率实现了研究区Ca O含量反演。通过利用LPI Apollo17月岩(壤)样品实际Ca O含量分析数据对反演结果进行精度评价,发现8组反演值与实际值的相对误差最小为1.77%,最大为9.29%,均方根误差为0.767。研究结果表明,使用发射率进行Ca O含量反演方法可行,为利用Clementine热红外数据对月表矿物成分含量定量反演提供一种新的思路。     

变质作用P—T—t轨迹若干问题评述

着重介绍了目前变质作用P－T─t轨迹研究在变质作用温压确定、变质作用不同阶段时间标定、变质作用动态演化过程的组构标志、变质作用演化热模拟以及变质作用P─T─t轨迹与大地构造环境之间关系等方面所存在的若干问题。     

福建省滨海火电厂地质灾害问题及风险控制探讨

滨海火力发电厂工程主要包括厂区建筑、码头、管道、取排水、填海和贮灰场等工程。其主要面临着福建省海岸带构造运动、断裂及地震活动、港湾淤积、海底滑坡、软土地基、海底活动地貌、基岩不均匀风化以及人类工程活动等主要的灾害性地质因素。通过对这些因素潜在的致灾特点分析，提出了滨海火电厂地质灾害风险控制应包括选址阶段地质灾害风险回避、设计施工阶段地质灾害风险处理及运行阶段地质灾害风险监控等3方面。地质灾害风险评估是滨海火电厂地质灾害风险控制的首要任务。针对滨海电厂工程的特点，评估内容应着重于地质灾害危险性评估及易损性评估。选址阶段地质灾害风险回避主要是对构造不稳定的回避。地质灾害风险处理主要是电厂工程的基础处理及管道抗冲刷处理。电厂运行阶段地质灾害风险监控主要是对建筑物基础稳定性及海域冲淤变化的监控。     

Thermal analysis in the laser-heated diamond anvil cell

A new technique actively controls thermal radiation and monitors sample properties during laser-heating in a diamond anvil cell. The technique can be described as a qualitative application of thermal analysis. Discontinuities in temperature, laser power, visible thermal radiation, or in their derivatives as functions of time can be associated with the enthalpy of phase transitions (such as melting) or with changes in maternal properties (such as emissivity).The technique is illustrated with melting experiments on iron-magnesium-silicate perovskite. Temperature corrections associated with these experiments are discussed and the results are briefly reviewed.