Impact of neutron star oscillations on the accelerating electric field in the polar cap of pulsar     

A. N. Timokhin 《Astrophysics and Space Science》2007,308(1-4):345-351

Pulsar “standard model”, that considers a pulsar as a rotating magnetized conducting sphere surrounded by plasma, is generalized to the case of oscillating star. We developed an algorithm for calculation of the Goldreich-Julian charge density for this case. We consider distortion of the accelerating zone in the polar cap of pulsar by neutron star oscillations. It is shown that for oscillation modes with high harmonic numbers (l,m) changes in the Goldreich-Julian charge density caused by pulsations of neutron star could lead to significant altering of an accelerating electric field in the polar cap of pulsar. In the moderately optimistic scenario, that assumes excitation of the neutron star oscillations by glitches, it could be possible to detect altering of the pulsar radioemission due to modulation of the accelerating field. This work was partially supported by RFBR grant 04-02-16720, and by the grants N.Sh.-5218.2006.2 and RNP-2.1.1.5940.  相似文献   

A three-dimensional numerical method for modelling weakly ionized plasmas     

Stephen O'Sullivan  Turlough P. Downes 《Monthly notices of the Royal Astronomical Society》2007,376(4):1648-1658

Astrophysical fluids under the influence of magnetic fields are often subjected to single- or two-fluid approximations. In the case of weakly ionized plasmas, however, this can be inappropriate due to distinct responses from the multiple constituent species to both collisional and non-collisional forces. As a result, in dense molecular clouds and protostellar accretion discs, for instance, the conductivity of the plasma may be highly anisotropic leading to phenomena such as Hall and ambipolar diffusion strongly influencing the dynamics.
Diffusive processes are known to restrict the stability of conventional numerical schemes which are not implicit in nature. Furthermore, recent work establishes that a large Hall term can impose an additional severe stability limit on standard explicit schemes. Following a previous paper, which presented the one-dimensional case, we describe a fully three-dimensional method which relaxes the normal restrictions on explicit schemes for multifluid processes. This is achieved by applying the little-known Super TimeStepping technique to the symmetric (ambipolar) component of the evolution operator for the magnetic field in the local plasma rest frame, and the new Hall Diffusion Scheme to the skew-symmetric (Hall) component.  相似文献   

Hardening of Thermal Photons Through Inverse Compton Scattering in Strong Magnetic Fields     

YiXu Hong－HuaXu 《中国天文和天体物理学报》2001,1(5):411-420

A new spectrum function is obtained by use of the Compton scattering cross section in the laboratory frame dervied earlier. This spectrum function, besides some modifications in the coefficients of the resonant term, contains also a non-resonant term which is inversely proportional to the square of the magnetic field. Based on this spectrum function, the hardening of thermal photons through inverse Compton scattering by relativistic electron beams on the surface of a strongly magnetized neutron star is investigated. Two new features are found. First, there is a maximum scattered photon energy for a given resonant scattering, beyond which resonance disappears. This maximum depends on the electron energy and the magnetic field, but is independent of the incident photon energy. Second, Beyond each resonant scattering, there is a high-energy tail, resulting from non-resonant scattering. It is also found that all the tails have a common upper limit which is the highest scattered photon energy for the given incident photon and electron energies. These two new features are absent in the Monte Carlo simulations and therefore, may have physical implications for γ-ray emissions.  相似文献   

The populations of comet-like bodies in the Solar system     

J. Horner  N. W. Evans  M. E. Bailey  D. J. Asher 《Monthly notices of the Royal Astronomical Society》2003,343(4):1057-1066

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Multidimensional numerical scheme for resistive relativistic magnetohydrodynamics     

Serguei S. Komissarov 《Monthly notices of the Royal Astronomical Society》2007,382(3):995-1004

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深层—超深层碎屑岩储层非均质性特征与油气成藏模式     

罗晓容  杨海军  王震亮  张立强  张立宽  雷裕红  周路  张宝收  严一鸣  曹斌风  刘志达 《地质学报》2023,97(9):2802-2819

深层—超深层地质条件下,储层的孔渗物性特征和流体动力连通关系决定了油气在储层中的流动状态,这也就决定了油气运移的动力条件和聚集成藏的机理与过程。本文基于对深层—超深层碎屑岩储层结构非均质性的研究,认识深层—超深层油气运聚成藏机制和过程,总结油气多期复合成藏模式,探索深层—超深层油气分布规律。碎屑岩储层普遍存在强烈的非均质性,受到沉积结构构造及成岩作用控制,表现出空间结构性特征,在埋藏至深层—超深层的过程中经历了差异性的成岩演化和油气充注。结构非均质性储层中的油气总体向上倾方向运移,受储层中砂体分布、隔夹层结构以及连通方式的影响,油气运移路径的分布极不均匀,在储层中任何部位都可能聚集,并可能继续运移到有利圈闭中富集。在深埋过程中,多期多幕的构造变动促使深层—超深层储层中已聚集的油气向着上倾方向运移调整,或沿着断裂向上运移调整至中—深层与之相关的有效储层中运移、聚集。深层—超深层勘探具有更为广泛的目标选择,洼陷区和斜坡区都可能成为有利勘探区域。现实的深层—超深层油气勘探新领域包括：构造高点油气藏向供源方向的拓展,深层—超深层烃源由断裂调整至中深层—超深层的次生油气聚集,深层—超深层与油气源...  相似文献   

Numerical simulations for MHD coronal seismology     

David James Pascoe 《中国天文和天体物理学报》2014,(7):805-830

Magnetohydrodynamic（MHD） processes are important for the transfer of energy over large scales in plasmas and so are essential to understanding most forms of dynamical activity in the solar atmosphere. The introduction of transverse structuring into models for the corona modifies the behavior of MHD waves through processes such as dispersion and mode coupling. Exploiting our understanding of MHD waves with the diagnostic tool of coronal seismology relies upon the development of sufficiently detailed models to account for all the features in observations. The development of realistic models appropriate for highly structured and dynamical plasmas is often beyond the domain of simple mathematical analysis and so numerical methods are employed. This paper reviews recent numerical results for seismology of the solar corona using MHD.  相似文献   

Some issues in diagnostics of solar chromospheric magnetic fields with the Mg b2 line     

Xian-Yong Bai  Yuan-Yong Deng  Jiang-Tao Su  Guo-Ping Wang 《中国天文和天体物理学报》2014,(2):193-206

Up to now, exact measurements of chromospheric magnetic fields have not been as successful as those done in the photosphere. We are currently engaging in diagnostics of chromospheric magnetic fields with the Mg b2 line by employing the Multi-Channel Solar Telescope at Huairou Solar Observing Station. Therefore, how to improve accuracy in the measurement is the main issue of our present study. To this end, we first study linear calibration coefficients for longitudinal and transverse components of chromospheric fields, which vary with wavelength, in the case of a weak field assumption. Then the polarization crosstalk introduced by instruments is analyzed in detail with two numerical simulation methods. Comparisons of the po- larization signals between cases with and without correction are presented. The result indicates that polarization accuracy is greatly improved after crosstalk correction.  相似文献   

Axisymmetry vs. nonaxisymmetry of a Taylor‐Couette flow with azimuthal magnetic fields     

M. Gellert  G. Rüdiger 《Astronomische Nachrichten》2015,336(1):63-69

The instability of a supercritical Taylor‐Couette flow of a conducting fluid with resting outer cylinder under the influence of a uniform axial electric current is investigated for magnetic Prandtl number Pm = 1. In the linear theory the critical Reynolds number for axisymmetric perturbations is not influenced by the current‐induced axisymmetric magnetic field but all axisymmetric magnetic perturbations decay. The nonaxisymmetric perturbations with m = 1 are excited even without rotation for large enough Hartmann numbers (“Tayler instability”). For slow rotation their growth rates scale with the Alfvén frequency of the magnetic field but for fast rotation they scale with the rotation rate of the inner cylinder. In the nonlinear regime the ratio of the energy of the magnetic m = 1 modes and the toroidal background field is very low for the non‐rotating Tayler instability but it strongly grows if differential rotation is present. For super‐Alfv´enic rotation the energies in the m = 1 modes of flow and field do not depend on the molecular viscosity, they are almost in equipartition and contain only 1.5 % of the centrifugal energy of the inner cylinder. The geometry of the excited magnetic field pattern is strictly nonaxisymmetric for slow rotation but it is of the mixed‐mode type for fast rotation – contrary to the situation which has been observed at the surface of Ap stars. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The most distant quasar at z = 7.08: Probable retrograde rotation of an accreting supermassive black hole     

Yu. N. Gnedin  A. G. Mikhailov  M. Yu. Piotrovich 《Astronomische Nachrichten》2015,336(3):312-315

We estimate the value of the spin of the supermassive black hole (SMBH) of the high‐redshift quasar ULAS J112001.48 +064124.3 using new observational data for its mass, bolometric luminosity, and X‐ray spectrum. We show that, assuming equilibrium between the magnetic and the accretion gas pressures at the event horizon radius, the spin of the SMBH is negative. This result implies that the SMBH in this quasar is rotating retrograde with respect to the accretion disk. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献