Strong magnetic field in W75N OH maser flare     

V. I. Slysh  V. Migenes 《Monthly notices of the Royal Astronomical Society》2006,369(3):1497-1501

A flare of OH maser emission was discovered in W75N in 2000. Its location was determined with the Very Long Baseline Array (VLBA) to be within 110 au from one of the ultracompact H  ii regions, Very Large Array 2 (VLA2). The flare consisted of several maser spots. Four of the spots were found to form Zeeman pairs, all of them with a magnetic field strength of about 40 mG. This is the highest ever magnetic field strength found in OH masers, an order of magnitude higher than in typical OH masers. Three possible sources for the enhanced magnetic field are discussed: (i) the magnetic field of the exciting star dragged out by the stellar wind; (ii) the general interstellar field in the gas compressed by the magnetohydrodynamic shock; and (iii) the magnetic field of planets which orbit the exciting star and produce maser emission in gaseous envelopes.  相似文献   

On the influence of magnetic fields on level populations     

Z. Q. Qu  C. L. Xu  X. Y. Zhang  X. L. Yan  C. L. Jin 《Monthly notices of the Royal Astronomical Society》2006,370(4):1790-1796

The influence of magnetic fields on the energy level populations of atoms is firstly studied by analysing the Stokes profiles of Fe  i 6302.5 forming in the solar magnetized atmosphere, with the aid of a departure factor defined to evaluate the deviation from the normal Boltzmann distribution without a magnetic field. This factor is directly related to the ratio of line-source function to the continuum one. The relationship between the departure and the magnetic field reveals an effect that the magnetic field induces an exponential increase in the level population of the lower level of Fe  i 6302.5 (Landé factor   g = 2.5  ) with the field strength. This indicates that the magnetic field can cause the redistribution of populations of those levels whose Landé factors are non-zero. Therefore, this effect should be included in the calculation of the statistical equilibrium. Secondly, an experiment utilizing the Hg5461 line in the laboratory on the Earth is carried out to reveal that the exponential relation is independent of variations in temperature, and the excitation is completely magneto-induced. Finally, the exponential relation is explained by taking account of the magnetic energy in the Boltzmann distribution.  相似文献   

Strong asymmetry in stellar dynamos     

P. J. Bushby 《Monthly notices of the Royal Astronomical Society》2003,338(3):655-664

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Spine–sheath polarization structures in four active galactic nuclei jets     

A. B. Pushkarev  D. C. Gabuzda  Yu. N. Vetukhnovskaya  V. E. Yakimov 《Monthly notices of the Royal Astronomical Society》2005,356(3):859-871

We present the results of multifrequency (15 + 8 + 5 GHz) polarization Very Long Baseline Array (VLBA) observations of the three BL Lacertae objects 0745+241, 1418+546 and 1652+398 together with 5-GHz VLBI Space Observatory Programme (VSOP) observations of 1418+546 and 1.6- and 5-GHz VSOP observations of the blazar 1055+018. The jets of all these sources have polarization structure transverse to the jet axis, with the polarization E vectors aligned with the jet along the jet spine and 'sheaths' of orthogonal E vectors at one or both edges of the jet. The presence of polarization aligned with the jet near the 'spine' may indicate that the jets are associated with helical B fields that propogate outward with the jet flow; the presence of orthogonal polarization near the edges of the jet may likewise be a consequence of a helical jet B field, or may be owing to an interaction with the ambient medium on parsec scales. We have tentatively detected interknot polarization in 1055+018 with E aligned with the local jet direction, consistent with the possibility that the jet of this source is associated with a helical B field.  相似文献   

A Faraday rotation template for the Galactic sky     

Patrick Dineen  Peter Coles 《Monthly notices of the Royal Astronomical Society》2005,362(2):403-410

Using a set of compilations of measurements for extragalactic radio sources, we construct all-sky maps of the Faraday rotation produced by the Galactic magnetic field. In order to generate the maps, we treat the radio source positions as a kind of 'mask' and construct combinations of spherical harmonic modes that are orthogonal on the masked sky. As long as relatively small multipoles are used, the resulting maps are quite stable to changes in the selection criteria for the sources, and show clearly the structure of the local Galactic magnetic field. We also suggest the use of these maps as templates for cosmic microwave background (CMB) foreground analysis, illustrating the idea with a cross-correlation analysis between the Wilkinson Microwave Anisotropy Probe ( WMAP ) data and our maps. We find a significant cross-correlation, indicating the presence of a significant residual contamination.  相似文献   

塔里木盆地西部吐木休克断裂带的主要特征和构造演化   总被引：8，自引：5，他引：3       下载免费PDF全文

朱德丰  刘和甫  吴根耀 《地质科学》2008,43(2):209-227

塔里木盆地西部的吐木休克断裂带是中央隆起(前身是晋宁期碰撞造山带)的次级单元巴楚断隆与北部坳陷的次级单元阿瓦提凹陷之间的分界。本文以大量的地质和地球物理证据,证明它是一条内部结构复杂且切穿地壳的深断裂。结合区域构造演化恢复了断裂发育史,指出它经历过三期重大的冲断活动,分别发生在加里东期、海西期和新近纪。新近纪的冲断与巴楚断隆的南界断裂带有相同的构造样式,可分为两幕:中新世的冲断受制于南天山前陆冲断带的向南扩展,更新世的冲断主要受制于西昆仑前陆冲断带的向北扩展。吐木休克断裂带的东西走向段和北西走向段的构造特征尚有若干差异,前者在加里东期活动较强,反映了构造的继承性;北西走向段则是加里东期出现的新生构造,在海西期进一步发展,更新世时因被卷入西昆仑的前陆冲断作用,表现出强烈而复杂的变形。  相似文献   

高精度新方法测量计算船舶磁场分布     

陈芸  赵培聪  顾新宏  曹全林  罗法贵  王硕儒 《海洋与湖沼》1995,26(5):480-487

将高精度质子磁探仪和位场变换理论用于测量计算船舶磁场，以研究其在海洋中的分布。由质子磁探仪实测海面上１０ｍ处磁场的模（船的磁场与地磁场矢量的和的绝对值），用位场变换理论计算出船的磁场三个分量在水面和水下的分布；并采用一系列有效措施，提高计算速度和结果的精度。将该方法和磁球理论严格解比较，在ｚ＝０面上误差小于０．１％，在ｚ＝－２０ｍ面上误差小于１％；还给出船的磁场强度在船的纵横向的分布曲线和平面立体  相似文献   

Tectonic core of a sedimentary drift: a potential ridge propagation feature beneath the Blake Outer Ridge     

Dayton Dove  Steven C. Jaume  Erin Beutel 《Marine Geophysical Researches》2007,28(1):1-11

The Blake Outer Ridge is a 480–kilometer long linear sedimentary drift ridge striking perpendicular to the North American coastline. By modeling free-air gravity anomalies we tested for the presence of a crustal feature that may control the location and orientation of the Blake Outer Ridge. Most of our crustal density models that match observed gravity anomalies require an increase in oceanic crustal thickness of 1–3 km on the southwest side of the Blake Outer Ridge relative to the northeast side. Most of these models also require 1–4 km of crustal thinning in zone 20–30 km southwest of the crest of the Blake Outer Ridge. Although these features are consistent with the structure of oceanic fracture zones, the Blake Outer Ridge is not parallel to adjacent known fracture zones. Magnetic anomalies suggest that the ocean crust beneath this feature formed during a period of mid-ocean ridge reorganization, and that the Blake Outer Ridge may be built upon the bathymetric expression of an oblique extensional feature associated with ridge propagation. It is likely that the orientation of this trough acted as a catalyst for sediment deposition with the start of the Western Boundary Undercurrent in the mid-Oligocene.  相似文献   

南海海盆磁异常理论剖面的计算和磁条带的初步分析     

王述功  高仰 《海洋科学》1990,14(6):9-15

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磁偶源2.5维瞬变电磁场全空间FDTD数值模拟   总被引：1，自引：0，他引：1  

杨海燕  岳建华 《物探与化探》2008,32(3):326-330

为解决模拟瞬变电磁场在3维介质中传播出现的计算量大、对计算机要求高等问题,使用了3维磁偶极源来模拟2维均匀介质和层状介质中方形和薄板低阻体的全空间响应特征。模拟中使用了时域有限差分法,采用非均匀网格和时间步长,分析了瞬变电磁场在均匀介质和层状介质中的传播规律,以及巷道和交界面对场的影响特征,为解释全空间均匀介质和层状介质TEM异常提供参考。  相似文献