Gladstone–Dale relationship—Application for tektites     

Ulrike Rantzsch  Gert Kloess  Jan-Michael Lange  Thomas Witzke 《Chemie der Erde / Geochemistry》2011,71(2):197-199

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Destabilization of hydrodynamically stable rotation laws by azimuthal magnetic fields     

Günther Rüdiger  Rainer Hollerbach  Manfred Schultz  Detlef Elstner 《Monthly notices of the Royal Astronomical Society》2007,377(4):1481-1487

We consider the effect of toroidal magnetic fields on hydrodynamically stable Taylor–Couette differential rotation flows. For current-free magnetic fields a non-axisymmetric   m = 1  magnetorotational instability arises when the magnetic Reynolds number exceeds   O (100)  . We then consider how this 'azimuthal magnetorotational instability' (AMRI) is modified if the magnetic field is not current-free, but also has an associated electric current throughout the fluid. This gives rise to current-driven Tayler instabilities (TIs) that exist even without any differential rotation at all. The interaction of the AMRI and the TI is then considered when both electric currents and differential rotation are present simultaneously. The magnetic Prandtl number Pm turns out to be crucial in this case. Large Pm have a destabilizing influence, and lead to a smooth transition between the AMRI and the TI. In contrast, small Pm have a stabilizing influence, with a broad stable zone separating the AMRI and the TI. In this region the differential rotation is acting to stabilize the TIs, with possible astrophysical applications (Ap stars). The growth rates of both the AMRI and the TI are largely independent of Pm , with the TI acting on the time-scale of a single rotation period, and the AMRI slightly slower, but still on the basic rotational time-scale. The azimuthal drift time-scale is ∼20 rotations, and may thus be a (flip-flop) time-scale of stellar activity between the rotation period and the diffusion time.  相似文献   

Solar coronal heating by magnetic cancellation – II. Disconnected and unequal bipoles     

B. von Rekowski  C. E. Parnell  E. R. Priest 《Monthly notices of the Royal Astronomical Society》2006,369(1):43-56

Two-dimensional numerical magnetohydrodynamic simulations of a cancelling magnetic feature (CMF) and the associated coronal X-ray bright point (XBP) are presented. Coronal magnetic reconnection is found to produce the Ohmic heating required for a coronal XBP. During the BP phase where reconnection occurs above the base, about 90–95 per cent of the magnetic flux of the converging magnetic bipole cancels at the base. The last ≈5 to 10 per cent of the base magnetic flux is cancelled when reconnection occurs at the base. Reconnection happens in a time-dependent way in response to the imposed converging footpoint motions. A potential field model gives a good first approximation to the qualitative behaviour of the system, but the magnetohydrodynamics (MHD) experiments reveal several quantitative differences: for example, the effects of plasma inertia and a pressure build-up in-between the converging bipole are to delay the onset of coronal reconnection above the base and to lower the maximum X -point height.  相似文献   

Turbulent dynamo in asymptotic giant branch stars     

Noam Soker  Essam Zoabi 《Monthly notices of the Royal Astronomical Society》2002,329(1):204-208

Using recent results on the operation of turbulent dynamos, we show that a turbulent dynamo may amplify a large-scale magnetic field in the envelopes of asymptotic giant branch (AGB) stars. We propose that a slow rotation of the AGB envelope can fix the symmetry axis, leading to the formation of an axisymmetric magnetic field structure. Unlike solar-type αω dynamos, the rotation has only a small role in amplifying the toroidal component of the magnetic field; instead of an αω dynamo we propose an α ² ω . The magnetic field may reach a value of     , where B _e is the equipartition (between the turbulent and magnetic energy densities) magnetic field. The large-scale magnetic field is strong enough for the formation of magnetic cool spots on the AGB stellar surface. The spots may regulate dust formation, and hence the mass-loss rate, leading to axisymmetric mass loss and the formation of elliptical planetary nebulae (PNe). Despite its role in forming cool spots, the large-scale magnetic field is too weak to play a dynamic role and directly influence the wind from the AGB star, as required by some models. We discuss other possible problems in models where the magnetic field plays a dynamic role in shaping the AGB winds, and argue that they cannot explain the formation of non-spherical PNe.  相似文献   

The significance of stretching lineations in terms of progressive deformation and finite strain     

Benoit Ildefonse  Jean-Michel Caron 《Geodinamica Acta》2013,26(3):161-170

Abstract

For a given increment of deformation, stretching lineations can be defined either by old grains or by new grains.

Progressive strain accumulated in a matrix causes reorientation of old grains. The velocity field acting within a grain depends on the degree of non-coaxiality of the progressive strain in the matrix, and on the competence contrast between grain and matrix (e.g. Lister & Williams, 1983). Deformed populations of old grains do not systematically track the principal directions of finite stretch; this depends on the mechanical behavior of the grains. On the other hand, these populations may be good markers of finite strain magnitude, provided that the initial distribution is known.

In contrast, the statistical shape orientation distribution of population of new grains cannot be related in a simple way to the finite strain magnitude, but their preferred orientation is considered to be the best indicator of the principal directions of finite stretch.

An example is considered from the schistes lustrés near Kenestrelle (Val Chisone, Western Alps), where the observed mineral lineation is attributed to a late E-W stretching event in the alpine orogenic history.  相似文献   

安徽池州马头铜钼矿容矿构造特征及构造应力场浅析          下载免费PDF全文

霍明宇  王莹  解国爱  等 《江苏地质》2013,37(2):284-291

研究区位于安徽池州市梅村镇西峰庙—马头平移断层东北端,该处岩体和围岩的内外接触带区域发育了一中型铜钼矿.分析了研究区铜钼矿赋存条件和容矿构造的发育特征,统计了容矿节理的产状,整理绘制出成矿期研究区的构造应力场分布图.认为研究区内的容矿节理以张性节理为主,经极射赤平投影后得到的优势产状为285°∠87°,容矿节理和主断裂产状基本一致.研究区内构造应力场最大主应力轴(σ1)的方位为15°,最小主应力轴(σ3)的方位为105°,倾角近水平.此构造应力场与燕山晚期中国东部构造应力场一致,最大主应力均为NNE-SSW方向.在此区域构造应力场的控制下,形成了区内广泛发育的NNE-SSW向、具走滑性质的断层以及张性节理.  相似文献   

Magnetic fields of accretion disks and outflows in prograde and retrograde black holes     

Yu.N. Gnedin  M.Yu. Piotrovich  S.D. Buliga  T.M. Natsvlishvili 《Astronomische Nachrichten》2013,334(3):264-267

We show that for the accretion disk with equipartition between magnetic and radiative pressures, prograde black holes generate outflowing energy in jets more efficiently than retrograde black holes do. Both viscous radiative and irradiative disks provide more efficient outflow jets in the case of a prograde black hole than in the case of a retrograde black hole. Our results confirm the conclusion of Tchekhovskoy & McKinney (2012) that, for the same absolute value of the spin, prograde black holes with geometrically thick accretion disks generate outflows several times more efficiently than retrograde black holes do. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

风廓线雷达组网资料初步对比分析   总被引：7，自引：2，他引：5  

董丽萍  吴蕾  王令  赵城城  柳云雷 《气象》2014,40(9):1145-1151

以L波段探空雷达探测到的水平风为标准对全国风廓线雷达探测到的水平风的可信度进行评估,得到:风廓线雷达探测到的水平风在700 hPa高度以下与L波段探空雷达测风有较好的一致性;并且将风廓线雷达探测到的垂直速度与同址地面自动气象站观测到的1 h雨量进行相关性分析,得出垂直速度大小能很清楚地反映降水的开始、结束以及降水的强度;最后将全国风廓线雷达探测到的水平风进行组网对比分析,得出全国风廓线雷达探测得到的水平风在700 hPa高度下是可信的,风向可信度随探测高度的增加而增大。风速可信度随探测高度的增加而降低。  相似文献   

Influence of Collective Boulder Array on the Surrounding Time-averaged and Turbulent Flow Fields   总被引：1，自引：0，他引：1  

Achilleas G.TSAKIRIS  A.N.Thanos PAPANICOLAOU  Seyed M.HAJIMIRZAIE  James H.J.BUCHHOLZ 《山地科学学报》2014,(6):1420-1428

Arrays of large immobile boulders,which are often encountered in steep mountain streams,affect the timing and magnitude of sediment transport events through their interactions with the approach flow.Despite their importance in the quantification of the bedload rate,the collective influence of a boulder array on the approach timeaveraged and turbulent flow field has to date been overlooked.The overarching objective is,thus,to assess the collective effects of a boulder array on the time-averaged and turbulent flow fields surrounding an individual boulder within the array,placing particular emphasis on highlighting the bed shear stress spatial variability.The objective of this study is pursued by resolving and comparing the timeaveraged and turbulent flow fields developing around a boulder,with and without an array of isolated boulders being present.The results show that the effects of an individual boulder on the time-averaged streamwise velocity and turbulence intensity were limited to the boulder’s immediate vicinity in the streamwise（x/d c 〈 2-3） and vertical（z/d c 〈 1） directions.Outside of the boulder’s immediate vicinity,the time-averaged streamwise velocity was found to be globally decelerated.This global deceleration was attributed to the form drag generated collectively by the boulder array.More importantly,the boulder array reduced the applied shear stress exerted on theindividual boulders found within the array,by absorbing a portion of the total applied shear.Furthermore,the array was found to have a ＂homogenizing＂ effect on the near-bed turbulence thus significantly reducing the turbulence intensity in the near-bed region.The findings of this study suggest that the collective boulder array bears a portion of the total applied bed shear stress as form drag,hence reducing the available bed shear stress for transporting incoming mobile sediment.Thus,the effects of the boulder array should not be ignored in sediment transport predictions.These effects are encapsulated in this study by E  相似文献   

Domain structures in complex 3D magnetic fields     

R. M. Close  C. E. Parnell  E. R. Priest 《地球物理与天体物理流体动力学》2013,107(6):513-534

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