On the possibility of investigation of the magnetic field structure in subphotospheric layers of the Sun according to observations of sunspot torsional oscillations

A method of investigation of the magnetic field structure in subphotospheric layers of the Sun has been developed. The method is based on observations of the torisonal oscillations of single sunspots. Characteristics of the torsional oscillations have been obtained from observations of the longitudinal magnetic field and radial velocities of seven single sunspots in the photospheric line Fe I λ5253 Å. The parameters of the torsional oscillations and magnetic tubes in the deep layers have been determined. The radius of the cross section of a magnetic flux tube forming a sunspot is greatest near the Sun’s surface and is approximately equal to the radius of a sunspot umbra. Down to the deeper layers, it decreases quite quickly. The longitudinal electric current appearing in the magnetic tube changes direction. The typical time of the current changes is determined by the period of the torsional oscillations. The intensity of the longitudinal magnetic field in the tube increases with depth. The Alfven wave velocity averaged over the length of a magnetic tube is tens or hundreds of times less than this velocity in a sunspot umbra. It decreases with an increase in the period of oscillations. A decrease in the Alfven wave velocity leads to an increase in the twisting angle of magnetic field lines.     

The origin of our galactic magnetic field

A serious difficulty with the standard alpha‐omega theory of the origin of galactic magnetic fields involves the question of flux expulsion. This is intimately related to flux freezing. The alpha‐omega theory is shown in the context of the giant superbubble explosions that have a large impact on the physics of the interstellar medium. It is shown that superbubbles alone can duplicate the processes of the alpha‐omega dynamo and produce exponential growth of the galactic magnetic field. The possibility of the blow‐out of pieces of the magnetic field is discussed and it is shown that they have the potential to solve the flux‐expulsion problem. However, such an explanation must lead to apparent ‘gaps’ in the field in the galactic disc. These gaps are probably unavoidable in any dynamo theory and should have important observable consequences, one of which is an explanation for the escape of cosmic rays from the disc (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Population study of Pectinaria australis (polychaeta) in Tasman Bay

Grab samples were taken from a population of Pectinaria australis Ehlers in Tasman Bay, New Zealand, at intervals over a 2‐year period, March 1971 to March 1973. Settlement occurred in summer with the new recruits showing rapid growth and heavy mortality, giving an apparent life cycle time of 1 y. The population density varied greatly over short distances at one time, presumably due to random settlement of aggregations of larvae from the plankton.     

A high resolution relative paleointensity record from the Gerlache-Boyd paleo-ice stream region, northern Antarctic Peninsula

Herein we document and interpret an absolute chronological dating attempt using geomagnetic paleointensity data from a post-glacial sediment drape on the western Antarctic Peninsula continental shelf. Our results demonstrate that absolute dating can be established in Holocene Antarctic shelf sediments that lack suitable material for radiocarbon dating. Two jumbo piston cores of 10-m length were collected in the Western Bransfield Basin. The cores preserve a strong, stable remanent magnetization and meet the magnetic mineral assemblage criteria recommended for reliable paleointensity analyses. The relative paleomagnetic intensity records were tuned to published absolute and relative paleomagnetic stacks, which yielded a record of the last ∼8500 years for the post-glacial drape. Four tephra layers associated with documented eruptions of nearby Deception Island have been dated at 3.31, 3.73, 4.44, and 6.86 ± 0.07 ka using the geomagnetic paleointensity method. This study establishes the dual role of geomagnetic paleointensity and tephrochronology in marine sediments across both sides of the northern Antarctic Peninsula.     

Atténuation de l'intensité macrosismique pour la France métropolitaine : importance de l'intensité épicentrale

The main result of this work is to show that macroseismic intensity decay with distance strongly depends on the epicentral intensity. An attenuation law that takes this parameter into account is proposed for Metropolitan France, from the analysis of SISFRANCE macroseismic database. Such a model significantly reduces the difference between observed and theoretical intensities. A map of the attenuation variations is also set up for Metropolitan France. No major site effects are observed, but at a broad scale, young Alpine regions display a stronger attenuation than old Hercynian regions. To cite this article: P. Arroucau et al., C. R. Geoscience 338 (2006).     

温度变化对半刚性沥青路面裂缝的影响

半刚性基层沥青路面反射裂缝产生的原因之一是由半刚性基层温度变化引起的。根据路表代表性温度特征,运用有限元平面模型计算了裂缝尖端的应力强度因子,并对影响其大小的各因素进行了敏感性分析。结果表明,面层和基层的模量以及基层的温缩系数的增大会不同程度地导致裂缝尖端应力强度因子的增大,而面层的温缩系数对裂缝尖端应力 强度因子的影响并不明显。另外,增加面层厚度能有效地降低裂缝尖端应力强度因子,并提出碎石基层可有效地减缓路面反射裂缝的扩展的结论。     

内蒙古东乌旗哈巴特盖银多金属矿土壤地球化学异常特征

哈巴特盖测区1／5万土壤地球化学测量发现了4个异常区，多元素组合异常多分布在黑云母二长花岗岩的内、外接触带上，土壤地球化学异常特征显示本区成矿是多期次的，多元素组合异常在露头矿和盲矿上方均有出现，且异常连续、浓集中心明显，异常的强度和规模大，呈带状、宽带状或面状产出。     

中国中部全新世古地磁长期变和相对古强度研究

高分辨率的古地磁场长期变（Paleomagnetic Secular Variation,简称PSV）和相对古强度（Relative Paleomagnetic Intensity,简称RPI）研究是解决全新世湖泊研究定年难题的有效途径之一,也能为认识区域古地磁场的变化提供不可或缺的基础数据。然而,目前我国中部地区仍缺少年代序列可靠、时间分辨率在百年尺度的全新世PSV和RPI记录。先前的研究显示山西宁武公海全新世岩芯具有稳定的粉砂质粘土湖泊沉积,并通过25个（本文在全新世时段用到18个）陆生植物残体AMS ¹⁴C测年建立了可靠的高分辨率年代序列,为重建高质量的全新世PSV和RPI记录提供了良好条件。本文通过特征剩磁磁倾角的变化建立了PSV序列,利用磁化率（χ）、非磁滞剩磁（ARM）、饱和等温剩磁（SIRM）等环境磁学参数对特征剩磁强度（NRM_25mT）进行归一化,估算了RPI变化序列。结果表明,公海全新世湖泊沉积物的PSV和RPI记录与北半球其他湖泊和海洋记录具有较好的一致性,同时存在着显著的区域差异,可以作为我国中部地区湖泊沉积的对比曲线。