The mass of the Andromeda galaxy

This paper argues that the Milky Way galaxy is probably the largest member of the Local Group. The evidence comes from estimates of the total mass of the Andromeda galaxy (M31) derived from the three-dimensional positions and radial velocities of its satellite galaxies, as well as the projected positions and radial velocities of its distant globular clusters and planetary nebulae. The available data set comprises 10 satellite galaxies, 17 distant globular clusters and nine halo planetary nebulae with radial velocities. We find that the halo of Andromeda has a mass of together with a scalelength of 90 kpc and a predominantly isotropic velocity distribution. For comparison, our earlier estimate for the Milky Way halo is Although the error bars are admittedly large, this suggests that the total mass of M31 is probably less than that of the Milky Way . We verify the robustness of our results to changes in the modelling assumptions and to errors caused by the small size and incompleteness of the data set.
Our surprising claim can be checked in several ways in the near future. The numbers of satellite galaxies, planetary nebulae and globular clusters with radial velocities can be increased by ground-based spectroscopy, while the proper motions of the companion galaxies and the unresolved cores of the globular clusters can be measured using the astrometric satellites Space Interferometry Mission ( SIM ) and Global Astrometric Interferometer for Astrophysics ( GAIA ). Using 100 globular clusters at projected radii 20 R 50 kpc with both radial velocities and proper motions, it will be possible to estimate the mass within 50 kpc to an accuracy of 20 per cent. Measuring the proper motions of the companion galaxies with SIM and GAIA will reduce the uncertainty in the total mass caused by the small size of the data set to 22 per cent.     

Comparison of parallel group velocity of ECH waves with electron resonant velocity: Implication for electron diffusion by ECH waves

We have investigated the role of group velocity in the calculation of pitch-angle diffusion coefficients by electron cyclotron harmonic (ECH) waves in planetary magnetospheres. The assumption which is generally made that the parallel group velocity can be neglected in comparison with particle parallel velocity is examined in detail. It is found that for lowest harmonic band this assumption is quite good. It is found that in general it is not possible to ignore the parallel group velocity. However, for lowest harmonic band this assumption is quite good at low electron temperatures.     

Multiple stellar populations in the Sextans dwarf spheroidal galaxy?

We present wide-field     multiband ( BVI ) CCD photometry (down to     of the very low surface brightness dwarf spheroidal galaxy Sextans. In the derived colour–magnitude diagrams we find evidence suggesting the presence of multiple stellar populations in this dwarf spheroidal. In particular, we discover (i) a blue horizontal branch tail that appears to lie on a brighter sequence with respect to the prominent red horizontal branch and the RR Lyrae stars, very similar to what was found by Majewski et al. for the Sculptor dwarf spheroidal, (ii) hints of a bimodal distribution in colour of the red giant branch stars, (iii) a double red giant branch bump. All of these features suggest that (at least) two components are present in the old stellar population of this galaxy: the main one with     and a minor component around     . The similarity to the Sculptor case may indicate that multiple star formation episodes are also common in the most nearby dwarf spheroidals that ceased their star formation activity at very early epochs.     

川西—川中上三叠统地层对比及层序特征

川西上三叠统的须家河组与川中香溪群地层对比问题一直富有争议,而且由于前陆盆地的活动性、不对称性、沉积中心的迁移性等特点让川西—川中地层的划分对比变得更加复杂和困难。本次研究重在借助钻、测井资料的层序地层学分析,并结合露头剖面和地震资料,寻找全区可对比的标志性的层序界面,然后根据地层叠置样式、岩性、岩相的变化以及古生物资料等细分出低位、湖侵和高位体系域,在连井剖面层序对比的基础上建立了川西—川中以四级层序为单元的等时层序地层对比格架,提出了合理的须家河组与香溪群地层对比方案。这对盆地范围的岩相古地理重建、沉积体系的展布、有利相带的预测、油气资源评价等的研究都有重要意义。     

青藏高原纳木错西缘新元古代中期岩浆事件:对北拉萨地块起源的约束

本文报道了青藏高原北拉萨地块纳木错西缘变质辉长岩和花岗片麻岩的锆石U-Pb定年、岩石地球化学和锆石Hf同位素分析结果。锆石LA-ICP-MS定年结果表明,变质辉长岩和花岗片麻岩的原岩形成时代分别为720±6Ma和732±7Ma,相当于新元古代中期。变质辉长岩为钙碱性系列,具有Nb、Ta和Ti负异常,与岛弧玄武岩类似。变质辉长岩中锆石具有较高的εHf(t)值(+5. 2～+9. 7),应当是源自俯冲环境下相对亏损的地幔楔。花岗片麻岩原岩为I型花岗质岩石,并且具有较为均一的锆石εHf(t)值(-3. 3～+0. 3),可能形成于地壳内古元古代变质火成岩的部分熔融作用。结合区域地质资料,变质辉长岩和花岗片麻岩的原岩应当形成于新元古代中期的洋壳俯冲消减过程。北拉萨地块上的前寒武纪岩浆和变质记录与东非造山带的活动时限较为一致,因而北拉萨地块可能与东非造山带具有亲缘性。     

云县邦撒铁锰矿矿床成因探讨

铁锰矿产于新糖房背斜西翼南延澜沧江群中上部绢云石英片岩地层中,似层状、透镜状、囊状产出,矿床成因为沉积、变质铁锰矿床,其富集与表生氧化作用关系密切。     

华北克拉通南缘栾川群大红口组形成时代及其对新元古代构造演化的制约

华北克拉通南缘豫西地区保存有较为完整的变质结晶基底和中-新元古代沉积盖层,记录了重要的前寒武纪构造演化信息。近年来的年龄研究结果表明原认为是中-新元古代的汝阳群-洛峪群可能形成于中元古代早期(1. 75～1. 60Ga),而沿着华北克拉通南缘与秦岭造山带的拼合带(洛南-栾川断裂带)分布的新元古代盖层(主要为栾川群)的形成时代尚不明确。华北南缘新元古代栾川群主要由大理岩、片岩、千枚岩和碱性火山岩组成,其上部大红口组火山岩以碱性粗面质岩石为主,高硅富钾,与侵入到栾川群中下部的辉长岩构成典型的双峰式岩石组合。栾川群大红口组三个粗面岩样品的锆石U-Pb年龄分别为840±4Ma、845±5Ma和846±6Ma,结合已有的栾川群下伏地层最年轻的碎屑锆石年龄结果(～1000Ma),限定栾川群归属于新元古代早期(1000～840Ma)。大红口组岩浆岩的岩石组合和地球化学特征表明其形成于板内裂谷环境,根据区域构造资料以及前人的研究成果,栾川群火山岩与北秦岭同时期的岩浆活动共同指示了华北南缘与北秦岭在～845Ma均处于板内拉张阶段。     

内蒙古固阳渣尔泰山群层序地层学及其控制因素

渣尔泰山群是华北地台北缘中元古代裂陷槽沉积,主要为一套遭受绿片岩相区域变质的碎屑岩-碳酸盐岩建造。根据岩性、岩相、相序和不整合界面的综合研究,对这套地层进行了详细的层序界面分析和层序划分,识别出Ⅰ型、Ⅱ型和暴露-淹没复合型(Ⅲ型)3种类型层序界面,共划分出1个超层序、2个大层序和7个层序。总结了渣尔泰山群在碎屑滨岸、台缘碳酸盐岩与碎屑岩混积、碳酸盐台地、台前斜坡和陆棚盆地等不同古地理背景下的层序发育模式及其内部构成特征,并探讨了复合海平面变化、构造活动、沉积物供给、古地形等因素对层序形成和演化的控制作用。