中国软玉矿床类型及其矿物学特征

文章将中国11个产地的软玉（透闪石玉）矿床分为岩浆热液型和变质热液型两大类。其中岩浆热液型又根据侵入体的性质分为中酸性岩型、基性岩型、超基性岩型;变质热液型根据母岩特点分为碳酸盐岩型和蛇纹岩型,并从围岩和侵入岩体特征、矿体产状及大地构造背景等方面,对比分析了软玉矿床的相似性和差异性,总结了各产地软玉的品种、矿物成分、结构构造等矿物学特征;简单分析了软玉的找矿远景。     

Gravitational wave radiation from the coalescence of white dwarfs

We compute the emission of gravitational radiation from the merging of a close white dwarf binary system. This is done for a wide range of masses and compositions of the white dwarfs, ranging from mergers involving two He white dwarfs, through mergers in which two CO white dwarfs coalesce, to mergers in which a massive ONe white dwarf is involved. In doing so we follow the evolution of the binary system using a smoothed particle hydrodynamics code. Even though the coalescence process of the white dwarfs involves considerable masses, moving at relatively high velocities with a high degree of asymmetry we find that the signature of the merger is not very strong. In fact, the most prominent feature of the coalescence is that in a relatively small time-scale (of the order of the period of the last stable orbit, typically a few minutes) the sources stop emitting gravitational waves. We also discuss the possible implications of our calculations for the detection of the coalescence within the framework of future space-borne interferometers like LISA.     

巡天项目中的白矮星搜寻

首先,描述了白矮星的颜色特点和光谱型分类。白矮星是大多数恒星的终极状态,它会随着时间的推移而逐渐冷却。根据表面大气成分,它被划分成DA和DB等不同的光谱型。对某一颗白矮星来说,其光谱型分类可能会随着时间的推移而发生变化,这主要是由于其大气包层中的元素含量被对流过程改变引起的。为了对各类光谱型有更深入的研究,样本的完备性不可或缺。得益于近十几年来大型巡天项目的开展(如斯隆数字巡天、郭守敬望远镜的光谱巡天等),目前通过光谱证认的白矮星已超过4×10~4颗,其中绝大多数是H主导的DA型白矮星,另外还包含2 000多颗He主导的DB白矮星。此外,GALEX项目和GAIA卫星分别提供了有价值的白矮星紫外数据、空间位置和速度等信息。这些数据和信息对于白矮星的研究工作起到了非常大的促进作用。随后,对白矮星的大气参数、质量和运动学等内容作了简单的总结。人们利用模板匹配测量了绝大多数已知白矮星的大气参数,并获得了DB型白矮星的有效温度与紫外颜色间的线性关系。基于斯隆数字巡天的光谱数据,白矮星的质量分布和质量-半径关系也得到了较深入的研究。小质量白矮星具有较大的速度弥散,而大质量的则相反。最后,讨论了白矮星的形成和演化机制,这些机制都是基于现有的理论模型得到的。随着巡天项目中白矮星样本的增加,现有的模型会逐渐被修正和完善,新的模型也将随之建立。     

The neutrino emission due to plasmon decay and neutrino luminosity of white dwarfs

One of the effective mechanisms of neutrino energy losses in red giants, pre-supernovae and in the cores of white dwarfs is the emission of neutrino–antineutrino pairs in the process of plasmon decay. In this paper, we numerically calculate the emissivity due to plasmon decay in a wide range of temperatures 10⁷–10¹¹ K and densities (2 × 10²–10¹⁴) g cm⁻³. Numerical results are approximated by convenient analytical expressions. We also calculate and approximate by analytical expressions the neutrino luminosity of white dwarfs due to plasmon decay, as a function of their mass and internal temperature. This neutrino luminosity depends on the chemical composition of white dwarfs only through the parameter μ_e (the net number of baryons per electron) and is the dominant neutrino luminosity in all white dwarfs at the neutrino cooling stage.     

厦门中华白海豚的分布和数量

1994～1999年在厦门海域进行84航次中华白海豚船只跟踪和照像,记录392只次。设20个监视站,进行239个月的逐日观察,记录12624只次。整个厦门海域700km2均有中华白海豚分布,它可溯河至近淡水的河道,但不游出外海。厦门西港和同安湾口内的近岸最多,跃出海面的次数有明显的季节差异,4～5月最多。厦门海域中华白海豚数量估计不足100只,仅40只左右有确切记录。种群数量目前仍有减少趋势,因而应就地和迁地保护并举,加强对这种国家一级保护物种的保护。     

A spatially resolved 'inside-out' outburst of IP Pegasi

We present a comprehensive photometric data set taken over the entire outburst of the eclipsing dwarf nova IP Peg in 1997 September/October. Analysis of the light curves taken over the long rise to the peak-of-outburst shows conclusively that the outburst started near the centre of the disc and moved outwards. This is the first data set that spatially resolves such an outburst. The data set is consistent with the idea that long rise times are indicative of such 'inside-out' outbursts. We show how the thickness and the radius of the disc, along with the mass transfer rate, change over the whole outburst. In addition, we show evidence of the secondary and the irradiation thereof. We discuss the possibility of spiral shocks in the disc; however, we find no conclusive evidence of their existence in this data set.     

On the parallax of WD 0346++246: a halo white dwarf candidate

We present a parallax measurement for the very cool degenerate WD 0346+246, the serendipitous discovery of which was reported by Hambly et al. We find an absolute parallax of 36±5 mas, yielding a distance estimate of 28±4 pc. The resulting absolute visual magnitude of the object is M _V =16.8±0.3, making it the second-lowest luminosity white dwarf currently known. We use the distance estimate and measured proper motion to show that the object has kinematics consistent with membership of the Galactic halo. WD 0346+246 is therefore by far the coolest and least luminous of only a handful of plausible halo white dwarf candidates. As such, the object has relevance to the ongoing debate concerning the results of microlensing experiments and the nature of any baryonic dark matter component to the Galactic halo residing in stellar remnants.     

不同颜色青海软玉微观形貌和矿物组成特征

青海软玉颜色丰富,近年来对青海软玉矿物学的研究不少,但针对不同颜色青海软玉矿物学特征的研究还存在欠缺。本文利用偏光显微镜、扫描电子显微镜、电子探针及粉晶X射线衍射仪器,从透闪石微形貌特征、微观结构、矿物组成及结晶度四个方面,研究了青海软玉颜色与矿物学特征的对应关系。结果表明:白玉、烟青玉、糖玉中透闪石主要为纤维状,显微纤维变晶结构,结晶度为96. 12%～96. 88%;青白玉和翠青玉中透闪石主要为叶片状,显微叶片变晶结构,结晶度为97. 35%,97. 32%;青玉和碧玉中透闪石主要为叶片状,显微叶片-隐晶质变晶结构,结晶度为95. 48%,95. 29%;黄玉中透闪石主要为柱状,显微柱状变晶结构,结晶度为97. 84%。青海软玉主要组成矿物均为透闪石,含量在95%以上,部分次要矿物如翠青玉中的榍石、黄玉中的钙长石、青玉中的菱镁矿、碧玉中的铬铁矿、糖玉中的斜黝帘石只出现在特定颜色的青海软玉样品中。研究认为不同颜色青海软玉矿物学特征确实存在差异,这些特征为研究不同颜色青海软玉成矿环境及成矿条件提供了科学依据。     

Relation of Velocity Distribution and Mass for DA White Dwarfstwo

White dwarfs are the evolutionary endpoint of the low-and-medium mass stars. In the studies of white dwarfs, the mass of white dwarf is an important physical parameter. In this paper, we give an analysis about the velocity distribution of DA white dwarfs in the Sloan Digital Sky Survey (SDSS), and hope to find the relation between mass and velocity distribution of white dwarfs. We get the radial velocity and tangential velocity of every DA white dwarf according to their proper motion and spectral shift. Through analyzing the velocity distribution of DA white dwarfs, we find that the small-mass white dwarfs, which are produced from the single-star evolution channel, have a relatively large velocity dispersion.