Li Be B Energetics and Cosmic Ray Origin

Three different models have been proposed for LiBeB production bycosmic rays: the CRI model in which the cosmic rays areaccelerated out of an ISM of solar composition scaled withmetallicity; the CRS model in which cosmic rays with compositionsimilar to that of the current epoch cosmic rays are acceleratedout of fresh supernova ejecta; and the LECR model in which adistinct low energy component coexists with the postulated cosmicrays of the CRI model. These models are usually distinguished bytheir predictions concerning the evolution of the Be and Babundances. Here we emphasize the energetics which favor the CRSmodel. This model is also favored by observations showing that thebulk (80 to 90%) of all supernovae occur in hot, low densitysuperbubbles, where supernova shocks can accelerate the cosmicrays from supernova ejecta enriched matter. This revised version was published online in July 2006 with corrections to the Cover Date.     

Hydrodynamic simulations of propagating warps and bending waves in accretion discs

We present the results of a study of propagating warp or bending waves in accretion discs. Three-dimensional hydrodynamic simulations were performed using smoothed particle hydrodynamics (SPH), and the results are compared with calculations based on the linear theory of warped discs.
We examine the response of a gaseous disc to an initially imposed warping disturbance under a variety of physical conditions. We consider primarily the physical regime in which the dimensionless viscosity parameter α < H r , where H r is the disc aspect ratio, so that bending waves are expected to propagate. We also performed calculations for disc models in which α > H r , where the warps are expected to evolve diffusively. Small-amplitude (linear) perturbations are studied in both Keplerian and slightly non-Keplerian discs, and we find that the results of the SPH calculations can be reasonably well fitted by those of the linear theory. The main results of these calculations are: (i) the warp in Keplerian discs when α < H r propagates with little dispersion, and damps at a rate expected from estimates of the code viscosity; (ii) warps evolve diffusively when α > H r ; (iii) the slightly non-Keplerian discs lead to a substantially more dispersive behaviour of the warps, which damp at a similar rate to the Keplerian case, when α < H r .
Initially imposed higher amplitude, non-linear warping disturbances were studied in Keplerian discs. The results indicate that non-linear warps can lead to the formation of shocks, and that the evolution of the warp becomes less wave-like and more diffusive in character.
This work is relevant to the study of the warped accretion discs that may occur around Kerr black holes or in misaligned binary systems, and is mainly concerned with discs in which α < H r . The results indicate that SPH can model the hydrodynamics of warped discs, even when using rather modest numbers of particles.     

Space weathering on the Moon: Patina on Apollo 17 samples 75075 and 76015

Abstract— We studied patinas on lunar rocks 75075 and 76015 from the Apollo collection using a multi-disciplinary approach, including scanning electron microscopy (SEM), energy dispersive x-ray spectrometry (EDS), transmission electron microscopy (TEM), wavelength-dispersive x-ray (WDS) mapping, Mössbauer spectroscopy, spectral reflectance, and microspectrophotometry. Based on SEM petrography, we have defined three textural types of patina: glazed, fragmental, and classic (cratered). The presence of classic patina is diagnostic of lunar samples that have been exposed directly to the space weathering environment. It is characterized by the presence of microcraters and glass pancakes and is the patina type studied by earlier workers. Classic patina is found on 76015 but not on 75075. Glazed patina is found on both 76015 and 75075, whereas fragmental patina is found only on 75075. The glazed and fragmental patinas on 75075 were probably formed as a result of relatively large nearby impacts; and although these two types of patina are not strictly the result of direct exposure to the space weathering environment, they are important because they affect the optical properties of the rocks. Field emission gun SEM (FE-SEM) of classic patina on 76015 shows evidence of possible solar wind sputtering erosion. Transmission electron microscope studies of 76015 reveal the presence of impact-generated deposits and solar flare particle tracks which, like microcraters and pancakes, are diagnostic of direct exposure to space weathering processes. The outermost surface of the 76015 patina consists of an amorphous rim very much like the rims found on individual lunar soil grains; this amorphous patina rim probably formed by similar processes of impact-generated vapor condensation and possible sputter deposition. Wavelength-dispersive x-ray element maps of polished thin sections of 75075 and 76015 indicate that patina compositions are poor indicators of the compositions and mineralogies of the rocks underlying them. On average, the reflectance spectra of patinas on both samples are slightly darker than those of their unweathered equivalents. Microreflectance measurements show that a thick patina can dramatically alter the optical properties of the rock on which it forms. The backscatter Mössbauer (BaMS) spectrum of a patina-covered surface of 76015 is very similar to that of an unweathered surface, indicating that the Mössbauer signal is generated from beneath the patina. Because BaMS “sees” through surface space-weathering effects to the underlying rock, this technique has great potential for use in robotic missions to other planetary bodies.     

从有孔虫分析西藏南部白垩纪海平面升降

白垩纪是地质历史中的最大海侵时期。海平面的升降改变了海洋的物理、化学及生物因素,从而影响了有孔虫的演化与发展。根据对有孔虫丰度、分异度及演化类型的研究,认为西藏白垩纪最大海侵时期形成于赛诺曼期与土仑期的界线附近。此后海平面总的处于下降趋势,只是在康尼亚克期至三冬期海平面又有回升。马斯特里赫特末期有孔虫的大量灭绝反映了白垩纪与第三纪界线事件的影响。     

热带气旋外围环流中次天气尺度系统及其与天气尺度系统相互作用的诊断分析

本文应用带通滤波的方法,分离出热带气旋外围环流中的天气尺度和次天气尺度系统。发现热带气旋外围强降水与低层次天气尺度系统的辐合关系相当密切。文中还计算了两种尺度系统间的动能和涡度转换。得出:在650hPa以上基本上是天气尺度系统向次天气尺度系统提供动能,在650hPa以下基本上是次天气尺度系统向天气尺度系统提供动能,整层积分的结果是天气尺度系统向次天气尺度系统提供动能。在900hPa和400hPa之间的涡度转换为次天气尺度系统向天气尺度系统转换,即涡度转换的结果是使得次天气尺度系统气旋性减弱,天气尺度系统气旋性增强。900hPa以下和400hPa以上则相反。整层积分的结果是次天气尺度系统向天气尺度系统提供正涡度。      

论CILa/CISm—CILa图解

通过对分离结晶作用和批式熔融作用C_l^y/C_l^x-C_l^y图解的数学分析,笔者认为,虽然C_l^La/C_l^sm-C_l^La图解在一定程度上能区分这两种不同岩浆作用过程,但是,Treuil等的解释是不完全的。直线的斜率和截距还极大地受参数C_o^x,C_o^y,D_x,D_y的影响。该图解并非总是有效。本文还给出了一般式C_l^y/C_l^x-C_l^y在其它方面的可能应用。     

青藏高原西部日土-普兰一带古构造应力值的估算

本文用超显微构造的位错密度法,估算了该地区6次构造事件的古构造应力值。尽管从现在的构造形变特征来看,不同构造事件都是沿近南北方向的伸展或挤压,但其形变强度各不相同,印支运动（晚三叠世）最强,平均差应力值达201MPa,四川运动（白垩纪—早第三纪早期）次之,为183MPa,其它各次构造运动均较弱,阿森特运动（前寒武纪末期）为101MPa,海西运动（早二叠世晚期）为121MPa,燕山运动（晚侏罗世）为130Mpa,喜马拉雅运动（中新世末期以来）为110MPa,加里东运动在本区大部分地方较弱,我们未采集到能反映其构造应力状态的样品。