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)     

High Spatial Resolution X-Ray Spectroscopy of Cas A with Chandra

We present high spatial resolution X-ray spectroscopy of the supernova remnant Cassiopeia A with the Chandra observations. The X-ray emitting region of this remnant was divided into 38 × 34 pixels of 10″× 10″ each. Spectra of 960 pixels were created and fitted with an absorbed two component non-equilibrium ionization model. From the results of the spectral analysis we obtained maps of absorbing column density, temperatures, ionization ages, and the abundances of Ne, Mg, Si, S, Ca and Fe. The Si, S and possibly Ca abundance maps show obvious jet structures, while Fe does not follow the jet but seems to be distributed perpendicular to it. The abundances of Si, S and Ca show tight correlations between one another over a range of about two dex. This suggests that they are ejecta from explosive Oburning and incomplete Si-buming. Meanwhile, the Ne abundance is well correlated with that of Mg, indicating them to be the ashes of explosive C/Ne burning. The Fe abundance is positively correlated with that of Si when the latter is lower than 3 times the solar value, and is negatively correlated when higher. We suggest that such a two phase correlation is due to the different ways in which Fe was synthesized.     

Circumstellar Na I and Ca II absorption lines of type Ia supernovae in the symbiotic scenario

The formation of circumstellar Na I and Ca II resonance absorption lines in a type Ia supernova is studied in the case where the supernova explodes in a binary system with a red giant. The model suggests a spherically symmetric wind and takes into account the nonstationary ionization and heating of the wind by X rays from the shock wave and by gamma rays from radioactive ⁵⁶Ni decay. For wind densities typical of a red giant, the expected optical depth of the wind in Na I lines is shown to be too small (τ < 10^?3) for their detection. Under the same conditions, the optical depth of the predicted Ca II 3934 Å absorption line is sufficient for its detection (τ > 0.1). It is concluded that the Na I and Ca II absorption lines detected in SN 2006X could not be formed in the red giant wind and are most likely related to clouds at distances exceeding the dust evaporation radius (r > 10¹⁷ cm). An upper limit for the rate of mass loss through a stationary wind with velocity u has been obtained from the absence of Ca II absorption lines in SN 2006X unrelated to the similar Na I components: ? < 10^?8 (u/10 km s^?1) M _⊙ yr^?1.     

Dynamo coefficients from local simulations of the turbulent ISM

Observations in polarized emission reveal the existence of large‐scale coherent magnetic fields in a wide range of spiral galaxies. Radio‐polarization data show that these fields are strongly inclined towards the radial direction, with pitch angles up to 35° and thus cannot be explained by differential rotation alone. Global dynamo models describe the generation of the radial magnetic field from the underlying turbulence via the so called α ‐effect. However, these global models still rely on crude assumptions about the small‐scale turbulence. To overcome these restrictions we perform fully dynamical MHD simulations of interstellar turbulence driven by supernova explosions. From our simulations we extract profiles of the contributing diagonal elements of the dynamo α ‐tensor as functions of galactic height. We also measure the coefficients describing vertical pumping and find that the ratio between these two effects has been overestimated in earlier analytical work, where dynamo action seemed impossible. In contradiction to these models based on isolated remnants we always find the pumping to be directed inward. In addition we observe that depends on whether clustering in terms of superbubbles is taken into account. Finally, we apply a test field method to derive a quantitative measure of the turbulent magnetic diffusivity which we determine to be ∼2 kpckms^–1. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

超新星爆发与暗晕中重子物质的丢失

讨论了在以冷暗物质为主的宇宙中,超新星爆发对矮星系演化的反馈作用。建立了星系的质量丢失模型,提出了理论模型与观测进行比较的方法。对数值计算结果的理论分析表明,当星系外围存在一个暗物质晕时,由超新星爆发引起的质量丢失虽然受到了极大的限制,却不像人们预期的那么困难。如果假定星系的形成红移为ｚ＝２～８,那么,在所选取的参数范围内,理论计算和观测结果是相符合的。这种定性上的符合显示出,星系的质量越小,它们就形成得越早．     

大厚度自重湿陷性黄土湿陷变形特性水分入渗规律及地基处理方法研究

为研究大厚度自重湿陷性黄土的湿陷变形特性、水分入渗规律以及地基处理合理方法等问题,选择典型大厚度自重湿陷性黄土场地,进行了布置沉降观测点和埋设水分计的浸水试验以及挤密桩、DDC（孔内深层强夯）桩地基处理试验。试验结果表明,在水分入渗过程中,深度22.5～25.0 m以上土体易发生湿陷,该深度以下土体则含水率增加缓慢,达不到湿陷起始含水率,不易发生湿陷,因此该深度考虑可作为现场湿陷性评价的临界深度,也可作为大厚度湿陷性黄土地区进行地基处理时可参考的地基处理下限深度。DDC桩间距为1.0～1.4 m时,无论从挤密系数还是湿陷系数都能满足规范要求;挤密桩15 m试验区域沉降量较小,但其剩余湿陷量任未满足要求,这也佐证了关于22.5～25.0 m深度难于发生湿陷的结论。试验成果可作为今后大厚度自重湿陷性黄土地区工程建设以及黄土规范进一步修订的参考。     

广西凭祥中三叠世盆地沉积特征与构造属性分析

凭祥中三叠世盆地位于印支地块与华南地块碰撞拼合的缝合带内,记录了沿华南地块南缘展布的古特提斯分支洋盆俯冲闭合、印支地块与华南地块碰撞拼合的过程。本文通过大比例尺实测地质剖面,详细测量了凭祥盆地沉积相序及其组合变化,分析了不同相序的沉积环境及其物源,并探讨了盆地构造属性。结果表明,凭祥盆地主要充填有深水盆地相、浊积扇相和三角洲相等不同环境的沉积物。中三叠世期间盆地呈现为一系列因碰撞拼合作用形成的构造高地间夹深谷的岩相古地理面貌。深水盆地相以发育大套深灰色泥页岩和裹夹碎屑流沉积为特征,碎屑流沉积发育于构造高地陡坡一侧。浊积扇相以发育槽模、正粒序、爬升波纹层理、包卷层理、双向交错层理、透镜状层理、平行层理为特征。三角洲相以发育大型板状交错层理、潮沟、厚层透镜状砂体和砖红色泥岩为特征,类似发育于俯冲汇聚环境下的牙买加型扇三角洲,可能发育于构造高地缓坡一侧。沉积作用分析表明,主要存在碎屑流、浊流等重力流作用,并识别出底流作用。古水流分析表明存在向南和向北两个方向的物质搬运。岩相学特征表明盆地砂岩成分成熟度和结构成熟度均较低,物源为再旋回造山带或碰撞造山带。本文研究结果认为：凭祥盆地是一个伴随古特提斯分支洋盆俯冲闭合而被强烈改造的残余弧前盆地,时空上与之相配套是北泗组岛弧型流纹斑岩。该弧盆系统可能于晚二叠世末开始发育,中三叠世末结束沉积充填,暗示印支地块和华南地块最终于中三叠世碰撞拼合。     

昔格达断裂晚第四纪活动特征及强震复发周期

利用冲沟、山脊等断错构造地貌的DEM影像资料和详实的野外踏勘,详细分析了昔格达断裂的晚第四纪活动特征。结果显示:断裂线两侧的河沟和山脊地貌呈"S"或反"Z"形或以多个首尾连接的"S"形雁列式斜列,断裂活动为左行左列式,断层上发育多个拉分盆地和断裂湖;该断裂最新活动时间晚于(12.83±1.09)ka,为全新世走滑活动断裂,倾滑分量不大,倾向总体西倾,且晚更新世以来的左旋走滑速率约为1.70 mm/a;依据断裂线地震遗迹及断裂活动特征,断裂强活动复发间隔大致为10~12 ka或更短。     

金伯利岩中铬铁矿原生表面特征成因类型及其成分特征

对金伯利岩中铬铁矿原生表面特征的成因做出了合理解释,并提出了４种成因类型;通过探讨铬铁矿原生表面特征,化学成分,含矿性之间的关系,初步建立了铬铁矿原生表面特征与金刚石含矿性之间的关系。