基于Google Earth影像分析区域性大型“X”共轭节理系统对宏观岩溶作用的控制

从黔南、桂北的航天遥感图像上可以清楚地看出,地表的宏观岩溶地貌明显地受控于区域性大型“X”共轭节理系统,此类节理构成一幅巨型的渗滤网,成为大气降水下渗的主要通道,从而导致被其穿透的岩石遭受溶蚀,形成以线性岩溶谷地为主体的岩溶景观。即水平地层分布区,呈片状“X”形网络结构;直立地层分布区,呈羽状条带结构。水体下渗至潜水面后,将主要沿“X”节理走向向当地最低侵蚀基准面排泄,从而形成复杂的地下管道网络系统。首次利用网上Google Earth影像研究喀斯特环境,解决了只能依赖航片和卫星照片才能研究地球地貌的瓶颈,这对地貌研究和喀斯特石漠化的研究和治理提供了廉价便利的影像材料。     

Spectroscopic evidence of charge exchange X‐ray emission from galaxies

What are the origins of the soft X‐ray line emission from non‐AGN galaxies? XMM‐Newton RGS spectra of nearby non‐AGN galaxies (including starforming ones: M82, NGC 253, M51, M83, M61, NGC 4631, M94, NGC 2903, and the Antennae galaxies, as well as the inner bulge of M31) have been analyzed. In particular, the Kα triplet of O VII shows that the resonance line is typically weaker than the forbidden and/or inter‐combination lines. This suggests that a substantial fraction of the emission may not arise directly from optically thin thermal plasma, as commonly assumed, and may instead originate at its interface with neutral gas via charge exchange. This latter origin naturally explains the observed spatial correlation of the emission with various tracers of cool gas in some of the galaxies. However, alternative scenarios, such as the resonance scattering by the plasma and the relic photo‐ionization by AGNs in the recent past, cannot be ruled out, at least in some cases, and are being examined. Such X‐ray spectroscopic studies are important to the understanding of the relationship of the emission to various high‐energy feedback processes in galaxies (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Charge‐exchange X‐ray emission at hot/cool gas interfaces

Charge‐transfer (CT) X‐ray emission may occur at interfaces between a partially neutral gas and gas possessing high ions, provided there is a relative motion between those two phases. The CTX surface brightness from distant objects must be taken into account if it is not far below other “classical” emission sources, especially the thermal emission from the hot phase. I discuss those conditions and potential spectroscopic or photometric diagnostics. I also mention potential indirect effects of the CT reactions by means of pickup ion production, acceleration and subsequent modification of interface and plasma properties (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Extragalactic X‐ray surveys: AGN physics and evolution

We review the most important findings on AGN physics and cosmological evolution as obtained by extragalactic X‐ray surveys and associated multiwavelength observations. We briefly discuss the perspectives for future enterprises and in particular the scientific case for an extremely deep (2–3 Ms) XMM survey. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Suzaku observations of clusters of galaxies

We review results of Suzaku observations of the intracluster medium of clusters of galaxies whose O, Mg, Si, S and Fe abundances have been measured with good accuracy due to the good energy resolution and low background. Metal massto‐light ratios were derived and we will discuss the origin of the metals. We also review the results of the search for bulk motion and hard X‐ray emission. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

X‐rays from young stars: A summary of highlights from the XMM‐Newton Extended Survey of the Taurus Molecular Cloud (XEST)

The XMM‐Newton Extended Survey of the Taurus Molecular Cloud (XEST) is a survey of the nearest large star‐forming region, the Taurus Molecular Cloud (TMC), making use of all instruments on board the XMM‐Newton X‐ray observatory. The survey, presently still growing, has provided unprecedented spectroscopic results from nearly every observed T Tauri star, and from ≈50% of the studied brown dwarfs and protostars. The survey includes the first coherent statistical sample of high‐resolution spectra of T Tauri stars, and is accompanied by an U ‐band/ultraviolet imaging photometric survey of the TMC. XEST led to the discovery of new, systematic X‐ray features not possible before with smaller samples, in particular the X‐ray soft excess in classical T Tauri stars and the Two‐Absorber X‐ray (TAX) spectra of jet‐driving T Tauri stars. This paper summarizes highlights from XEST and reviews the key role of this large project. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Atmospheric Reactive Nitrogen Cycle and Stable Nitrogen Isotope Processes: Progresses and Perspectives

Oxidized reactive nitrogen in the atmosphere mainly consists of nitrogen oxides (NO _X =NO+NO₂, NO₃) and nitric acid. The atmospheric cycling of NO _X influences the formation of ozone and hydroxyl radicals that are important for atmospheric oxidation capacity. Nitric acid, the final product of NO _X oxidation, not only is an important component of particulate pollutants, but also has a direct impact on the ecosystem through dry and wet deposition. The stable nitrogen isotope (δ¹⁵N) shows the potential to study reactive nitrogen cycle, and to trace the emission, transport and deposition of reactive nitrogen from local to global scales. Here, we reviewed previous studies using δ¹⁵N to investigate NO _X emission and atmospheric reactive nitrogen cycle, and discuss the uncertainties of δ¹⁵N signatures of different NO _X sources from two aspects: NO _X generation mechanism and NO _X collection methods. We also discussed the nitrogen isotope fractionation and the consequences during the conversions of NO _y molecules. We ended up with discussions on the possibility of using δ¹⁵N to trace NO _X emissions. Although there are still large uncertainties in quantifying and tracing NO _X emissions using nitrogen stable isotopes, such isotope tool is efficient enough to trace reactive nitrogen cycles in the atmosphere. On the basis of this, we proposed that we can combine atmospheric chemistry transmission models with isotope tracers to improve our understanding of regional and global atmospheric reactive nitrogen cycle regarding the fluxes of different emission sources, their atmospheric transformation, etc.     

深海管道钢的腐蚀疲劳裂纹扩展特性试验研究

采用侧壁开槽型CT试样,分别在空气和3.5%NaCl溶液中进行腐蚀疲劳裂纹扩展试验,研究海底管道用钢X65在海水腐蚀环境下的腐蚀疲劳裂纹扩展特性。为保证试样既能满足腐蚀疲劳试验机的夹具要求,又可控制裂纹沿直线方向扩展,采用侧壁开槽技术对CT试样进行改进;利用有限元软件ABAQUS,建立三维模型,验证了对于侧壁开槽型CT试样,可以采用ASTM标准推荐的应力强度因子表达式对改进后CT试样开展数值计算。利用YYF-50腐蚀疲劳试验装置开展试验,试验结果表明:和惰性环境相比,腐蚀环境不仅会加速X65钢的裂纹扩展速率,还会降低腐蚀疲劳体系下裂纹扩展的门槛值;在腐蚀体系下存在裂纹扩展的稳定阶段,可采用Paris公式对其腐蚀疲劳裂纹扩展速率进行预测。     

Comprehensive study of the drying behavior of Boom clay: Experimental investigation and numerical modeling

This paper presents a thermo‐hydro‐mechanical framework to model the drying behavior of Boom clay. First, the experimental campaign conducted Noémie Prime is briefly presented because it is used to validate the model. The data acquisition and processing is emphasized because of the use of X‐ray microtomography to be able to more accurately compare experimental and numerical strain fields. The different submodels are introduced. Numerical simulations are performed to illustrate the capability of the proposed model to reproduce the observed behavior. Finally, a comprehensive sensitivity study on several key model parameters associated with the water retention curve, and the permeability of the medium, is performed to get a better understanding of the physics behind the coupled model.     

A ‘superoutburst’ in XTEJ1118+480

I propose that the properties of the two outbursts observed in the X‐ray transient XTEJ1118+480 in 2000 are akin to superoutbursts of SU UMa stars. In these systems a ‘normal’ outburst immediately precedes a 5–10 times longer (‘super’) outburst. The optical light curve of the outbursts of XTEJ1118+480 is remarkably similar to that seen in some SU UMa stars, such as UVPer and TLeo, where the precursor outburst is distinct from the superoutburst, but the time scales are a factor of ∼15 different. The first outburst of XTEJ1118+480 was relatively short (∼1 month) while the second outburst was ∼5 times longer. During the second outburst superhumps were seen, a feature characteristic for superoutbursts. The gap of about a month between the two outbursts is longer in X‐rays with respect to the optical, a feature not previously recognized for X‐ray transients. Also in SU UMa stars the precursor outburst becomes more distinct at shorter wavelengths. Finally, I show that the time of appearance of the superhumps in XTEJ1118+480 is consistent with the expected superhump growth time, if the superhump mechanism was triggered during the first outburst. I conclude that the similarity in outburst behaviour in the two types of systems provides further support that a common mechanism is at work to start the long (‘super’) outbursts.