Waiting for the Big One: a new class of soft gamma-ray repeater outbursts?   总被引：1，自引：0，他引：1  

David Eichler 《Monthly notices of the Royal Astronomical Society》2002,335(4):883-886

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The influence of Hall drift on the magnetic fields of neutron stars     

Rainer Hollerbach †  Günther Rüdiger 《Monthly notices of the Royal Astronomical Society》2002,337(1):216-224

We consider the evolution of magnetic fields under the influence of Hall drift and Ohmic decay. The governing equation is solved numerically, in a spherical shell with   r _i / r _o = 0.75  . Starting with simple free-decay modes as initial conditions, we then consider the subsequent evolution. The Hall effect induces so-called helicoidal oscillations, in which energy is redistributed among the different modes. We find that the amplitude of these oscillations can be quite substantial, with some of the higher harmonics becoming comparable with the original field. Nevertheless, this transfer of energy to the higher harmonics is not sufficient to accelerate significantly the decay of the original field, at least not at the   R _B = O (100)  parameter values accessible to us, where this Hall parameter   R _B   measures the ratio of the Ohmic time-scale to the Hall time-scale. We do find clear evidence though of increasingly fine structures developing for increasingly large   R _B   , suggesting that perhaps this Hall-induced cascade to ever-shorter length-scales is eventually sufficiently vigorous to enhance the decay of the original field. Finally, the implications for the evolution of neutron star magnetic fields are discussed.  相似文献   

Dynamics of the solar tachocline – I. An incompressible study     

P. Garaud 《Monthly notices of the Royal Astronomical Society》2002,329(1):1-17

Gough & McIntyre have suggested that the dynamics of the solar tachocline are dominated by the advection–diffusion balance between the differential rotation, a large-scale primordial field and baroclinicly driven meridional motions. This paper presents the first part of a study of the tachocline, in which a model of the rotation profile below the convection zone is constructed along the lines suggested by Gough & McIntyre and solved numerically. In this first part, a reduced model of the tachocline is derived in which the effects of compressibility and energy transport on the system are neglected; the meridional motions are driven instead by Ekman–Hartmann pumping. Through this simplification, the interaction of the fluid flow and the magnetic field can be isolated and is studied through non-linear numerical analysis for various field strengths and diffusivities. It is shown that there exists only a narrow range of magnetic field strengths for which the system can achieve a nearly uniform rotation. The results are discussed with respect to observations and to the limitations of this initial approach. A following paper combines the effects of realistic baroclinic driving and stratification with a model that closely follows the lines of work of Gough & McIntyre.  相似文献   

长江三峡及邻区板内中强地震的孕震动力学分析     

张秋文 《大地测量与地球动力学》1994,(4)

本文在研究长江三峡及邻区地壳─上地幔结构和现今地壳重力场基础上，分析了该区板内中强地震的孕震动力学过程，探讨了整体上相对稳定的长江三峡及邻区孕育和发生中强地震的动力学机制，并提出了该区板内中强地震预测的动力学标志。  相似文献   

推覆构造滑脱层有限变形力学分析     

杨成永 《大地测量与地球动力学》1993,(4)

本文根据推覆构造滑脱层的变形特点,运用以S—R分解定理为基础的有限变形力学理论,研究了断坪与断坡滑脱层的变形场特征。用全量及增量方法逆解求出了变形滑脱层所受的边界外力;利用变形场与应力场的分析结果,给出了推覆构造在拆离时推覆席体的推移距离及作用推力的简捷计算公式。  相似文献   

Effects of applied stress on effective elastic anisotropy in cracked solids     

Evgenyi M. Chesnokov  Sergei V. Zatsepin 《Geophysical Journal International》1991,107(3):563-569

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Electric charge and magnetic flux on rotating black holes in a force-free magnetosphere     

Hyun KyuLee  Chul H.Lee  Maurice H. P. M.van Putten 《Monthly notices of the Royal Astronomical Society》2001,324(3):781-784

The electric charge on rotating black holes is calculated to be ∼ BJ in the force-free configuration of Ghosh, with a horizon flux of ∼ BM ². This charge is gravitationally weak for B ∼10¹⁵ G , so that the Kerr metric applies. Being similar to the electric charge of a magnetar, both electric charge and magnetic flux should be, in sign and order of magnitude, continuous during stellar collapse into a black hole. Extraction of the rotational energy from newly formed black holes may proceed by interaction with the magnetic field.  相似文献   

Magnetic flux separation in photospheric convection     

N. O. Weiss  M. R. E. Proctor  D. P. Brownjohn 《Monthly notices of the Royal Astronomical Society》2002,337(1):293-304

Three-dimensional non-linear magnetoconvection in a strongly stratified compressible layer exhibits different patterns as the strength of the imposed magnetic field is reduced. There is a transition from a magnetically dominated regime, with small-scale convection in slender hexagonal cells, to a convectively dominated regime, with clusters of broad rising plumes that confine the magnetic flux to narrow lanes where fields are locally intense. Both patterns can coexist for intermediate field strengths, giving rise to flux separation: clumps of vigorously convecting plumes, from which magnetic flux has been excluded, are segregated from regions with strong fields and small-scale convection. A systematic numerical investigation of these different states shows that flux separation can occur over a significant parameter range and that there is also hysteresis. The results are related to the fine structure of magnetic fields in sunspots and in the quiet Sun.  相似文献   

How Fast Could a Proto-pulsar Rotate?     

Ren-Xin Xu  Hong-Guang Wang  Guo-Jun QiaoDepartment of Astronomy  School of Physics  Peking University  Beijing 《中国天文和天体物理学报》2002,2(6)

According to two estimated relations between the initial period andthe dynamo-generated magnetic dipole field of pulsars, we calculate the statisticaldistributions of pulsar initial periods. It is found that proto-pulsars are very likelyto have rotation periods between 20 ms and 30 ms, and that most of the pulsarsrotate initially at a period ＜ 60 ms. Our result supports the asymmetric neutrinoemission model for pulsar kick.  相似文献   

Harmonic Structures of Gyrosynchrotron Radiation and Cyclotron Maser Instability     

Ai-Hua Zhou  Guang-Li Huang 《中国天文和天体物理学报》2001,1(4):365-371

1 INTRODUCTIONSolar microwave bursts are usually produced by dtherellt radiation mechanisxns: gyroresonance absorption, Coulomb brernsstrahlung of the thermal baCkground plasma, as well asgyrosynchrotron radiation of the nonihermal electrons (Hildebrandt et al. 1998). Meanwhile,cyclotron or synchrotron maser instabilities may be responsible for microwave spaaes, blips, andtype ill bursts (Wu 1985; Huang 1987; Huang et al. 1996; Huang 1998), which are usuajly superposed on the ambient mi…  相似文献