地质力学磁力模型试验中均匀梯度磁场的构建

地质力学磁力模型试验利用电磁力（场）模拟重力（场）的原理研究地质力学工程问题,采用的相似材料由铁磁材料与岩土体混合而成。铁磁材料在磁场中的受力方向和大小与所处空间的磁通密度梯度的大小和方向有关,为了模拟均匀的重力场,需要得到在一定空间范围内磁通密度梯度大小相同、方向单一的磁场。根据电磁学基本原理,构建了3种磁路形式以获得磁通密度梯度相对均匀的磁场,对磁力模型试验相似材料进行加载。对比3种磁路,在最佳试验区内开放式磁路对磁场的利用率更高,所以在电流相同条件下等到的磁通密度梯度的量值也更大。与另两种磁路形式相比,尽管半开放式磁路在重量和工作效率上的性能不及开放式和封闭式磁路,但其最佳试验空间的磁通密度梯度的均匀性最好,误差在5%以内,半开放式磁路可以作为地质力学磁力模型试验的磁场发生装置。     

Localization of magnetic reconnection from the differential characteristics of magnetic fields

Magnetic reconnection for arbitrary magnetic fields without null points is analyzed in the absence of plasma. A potential model field for four sources is considered. A method for the localization of probable reconnection regions using computable differential characteristics of magnetic fields is proposed. Some separator properties are examined, and separator regions are found for the best-known reconnection conditions.     

Solving the structural inverse problem of magnetic prospecting with respect to demagnetization for a two-layer medium model

The integral equations of the direct problem of magnetic prospecting with respect to demagnetization are derived for a two-layer medium model; a method of determining the intensity of a secondary magnetic field for the case of magnetizing by a static field, whose potential is a harmonic function, is described. The respective integral equations are written based on the theory of a simple layer potential. An iteration algorithm for solving the three-dimensional structural inverse problem of magnetic prospecting with respect to demagnetization for the sampled medium model is proposed based on the modified method of local corrections. Its numerical implementation is less computer-intensive than, for example, the gradient methods of nonlinear minimization, the sampling accuracy being equal. Note that problems of electric and magnetic prospecting with respect to demagnetization and thermometry are mathematically equivalent for stationary fields [1]. Therefore, the obtained results can be used in interpreting the data of these methods.     

Validate global mapping of internal lunar magnetic field

In this work, we report a global mapping of vector lunar magnetic field based on new method of separation of internal and external fields. The magnetic measurements collected during the lifetime of lunar prospector (LP) extended mission during 1999 were strongly disturbed by the solar wind, a period which coincided with a maximum of the 23 cycle activity. The multiscale wavelength external fields were analyzed using spherical harmonic transform. The external field determined by inversion was then removed from each magnetic field component for each half orbit. To map the vector magnetic crustal anomalies, all LP magnetometer data collected at low altitudes in the three different lunar environments: (1) geomagnetic tail, (2) solar wind, and (3) geomagnetic sheath were processed using this new approach. The results obtained using these selection criteria allow us to get a global coverage of the lunar surface by the vector magnetic field at variable spacecraft low altitudes. To validate our mapping, we have developed and applied a method based on properties of potential fields functions. This method can be used to determine both horizontal north and east components using only vertical component. The validated lunar internal magnetic measurements obtained at variable spacecraft altitudes were then continued to a common altitude of 30 km using an inverse method. This mapping confirms firstly the nature of the crustal sources of lunar magnetic field and clearly shows that the strongest concentrations of anomalies are associated with high albedo and/or located antipodal to large young basins (Orientale, Serenitatis, Imbrium, and Crisium) of age about 3.9 Ga.     

The theory of spontaneous emission by electrons during their motion along the quantizing magnetic field of a star

The quantum motion of non-relativistic and relativistic electrons in the presence of constant magnetic fields at the surfaces of magnetic stars, magnetic white dwarfs, and pulsars is considered. The quantizing magnetic-field strengths for charged particles with specified energies are determined. The quantum motion of these particles in a plane perpendicular to the magnetic field is accompanied by spontaneous radiation due to electron transitions from higher to lower discrete energy levels, right down to the ground state. In the non-relativistic case, this emission is monochromatic. In the non-relativistic case, various frequencies are emitted, but lie within an order of magnitude of each other. The electron kinetic energy along the magnetic field varies from zero to a maximum value, due to the one-dimensional character of the motion along the field, between each pair of potential barriers corresponding to the discrete energy levels. The results may be relevant to describing gamma-ray flares of pulsars.     

Sources of the global magnetic field of the Sun

Data on the global magnetic field (GMF) of the Sun as a star for 1968–1999 are used to determine the correlation of the GMF with the radial component of the interplanetary magnetic field (IMF) |B _r|; all data were averaged over a half year. The time variations in the GMF |H| are better correlated with variations in |B _r|; than the results of extrapolating the field from the “source surface” to the Earth’s orbit in a potential model based on magnetic synoptic maps of the photosphere. Possible origins for the higher correlation between the GMF and IMF are discussed. For both the GMF and IMF, the source surface actually corresponds to the quiet photosphere—i.e., background fields and coronal holes—rather than to a spherical surface artificially placed ≈2.5 R _⊙ from the center of the Sun, as assumed in potential models (R _⊙ is the solar radius). The mean effective strength of the photospheric field is about 1.9 G. There is a nearly linear dependence between |H| and |B _r|. The strong correlation between variations in |H| and |B _r| casts doubt on the validity of correcting solar magnetic fields using the so-called “saturation” factor δ^?1 (for magnetograph measurements in the λ 525.0 nm FeI line).     

The hanle effect in a turbulent magnetic field

Exact analytical expressions for the scattering phase matrix are presented for various models of a turbulent magnetic field having a symmetry axis in the solar atmosphere. The polarization of the scattered radiation in the plane of the scattering is shown to be virtually independent of the predominant direction of the turbulent magnetic field. The Hanle effect does not operate in a longitudinal magnetic field normal to the surface of the atmosphere, since the phase matrix has the form of a resonance phase matrix with zero magnetic field.     

A dynamo in a torus as an explanation of magnetic fields in the outer rings of galaxies

It is currently generally believed that magnetic fields in the disks of spiral galaxies are generated by the dynamo mechanism, which is based on the joint action of differential rotation and the alpha effect, associated with turbulent motions in the interstellar gas. Together with their disks, outer rings are also encountered in galaxies, where magnetic fields may be present. In earlier studies, the generation of magnetic fields has been described in a planar approximation, whose essence is that the size of rings perpendicular to the plane of the galaxy is much smaller than their size in the radial direction. However, it is plausible that these sizesmay sometimes be comparable, so that it would be more logical to suppose that a ring has a toroidal form. A model for a dynamo in a toroidal ring is constructed in this study. This model describes the magnetic field using two functions, corresponding to the toroidal component of the field and the part of the vector potential characterizing its poloidal component. The possible generation of magnetic field in various cases is shown, with both quadrupolar symmetry (close to the fields obtained in the planar approximation) and dipolar symmetry (when two layers with oppositely directed magnetic fields form in the ring). The parameter values for which the generation of fields with one or the other type of symmetry is possible are estimated. The results can also be used to describe the evolution of the magnetic fields in other toroidal astrophysical objects.     

New perspectives on Mars’ crustal magnetic field

The planet Mars lacks, today, a planetary, dynamic magnetic field, but strong, intense, localized magnetic fields of lithospheric origin, one to two orders of magnitude larger than the terrestrial lithospheric field, are present. This lithospheric magnetic field is the result of magnetization processes in the presence of a magnetic dynamo and of demagnetization processes after the dynamo shutdown, such as impact or volcanoes. This crude scenario can be more accurately specified by interpreting global and local models of the current magnetic field of Mars. Some specific areas are studied, including the intensely magnetized Terra Sirenum, as well as the magnetic anomaly associated with Apollinaris Patera. Magnetic minerals could be of primary and/or secondary origin; this latter would imply an early hydration of a basaltic crust. A scenario, in which Mars experienced a major polar wander due to the Tharsis bulge, prior to the cessation of its dynamo, is proposed and discussed.     

The electric fields of radio pulsars with asymmetric nondipolar magnetic fields

The effect of the curvature of open magnetic field lines on the generation of electric fields in radio pulsars is considered in the framework of a Goldreich-Julian model, for both a regime with a free outflow of electrons from the neutron-star surface and the case of a small thermoemission current. An expression for the electron thermoemission current in a strong magnetic field is derived. The electric field associated with the curvature of the magnetic flux tubes is comparable to the field generated by the relativistic dragging of the inertial frames.     

CSAMT测量中磁场对测量结果的影响

CSAMT的标量测量中常采用共磁道测量方式,即同步观测测量剖面上多个电道信号和垂直测量剖面的一个磁道信号,由此计算各测点的Cagniard视电阻率。因磁场测量位置的不同,势必对测量结果产生影响。计算了均匀半空间条件下不同测量位置的磁场强度,以及对视电阻率的影响;模拟了存在局部三维异常体时,赤道装置下不同位置的磁场对视电阻率的影响。结合野外实测资料分析认为,由磁场测量位置偏差引起的视电阻率误差难以校正,在实际工作中应尽量采用单电单磁的测量方式;当在大收发距且浅层电性结构单一的条件下,可以采用三电一磁的测量方式。研究对CSAMT标量测量方式的改进及实际勘查工作具有一定的指导意义。      

地质力学磁力模型试验原理及其在工程中的应用

地质力学磁力模型试验借鉴土工离心模型试验中利用离心力模拟重力的思想。在均匀梯度磁场中,掺有铁磁材料的相似材料会受到均匀的磁力作用,由此可以利用均匀的磁力场模拟重力场。根据电磁学基本原理和磁路设计原理,设计并制造了一台2 000匝线圈的均匀梯度磁场发生装置。该装置在220 V电压情况下,能够产生0～16 A电流,在1.2 m×1.2 m×1.0 m试验空间内,可将磁性相似材料的重度提高10～30倍。以锦屏一级电站左岸高陡边坡为例,进行地质力学磁力模型试验。试验结果表明,在一定的电流作用下,可以使模型所受体力的提高倍数达到相似比的要求,并与数值模拟结果进行了对比,试验结果与计算结果基本一致。在增加通电电流时,试验设备可以模拟边坡的超载过程,进而可以求出边坡的超载安全系数。     

Magneto-rotational instability in the accreting envelope of a protostar and the formation of the large-scale magnetic field

We investigate the role of the magnetic field in the collapse of a gas-dust cloud into a massive gravitating object. Observations of one such object (G31.41) indicate that the magnetic field has an hourglass shape oriented along the rotation axis of the matter, due to the freezing-in of the magnetic-field lines in the accreting matter. It is believed that accretion in stellar disks is associated with the transport of angular momentum from the center to the periphery, which could be initiated by large-scale vortex structures arising in the presence of unstable rotational flows of matter. The numerical simulations have established that the equilibrium configuration of a gas-dust disk rotating in a spherically symmetrical gravitational potential is subject to the development of strong instability in the presence of a weak magnetic field. It is shown that the development of instability leads to a transport of angular momentum to the disk periphery by large-scale vortex structures, together with the accretion of matter onto the gravitating object. The magnetic-field lines near the equator take on a chaotic character, but an hourglass configuration is observed near the rotation axis, in agreement with observations.     

最新的岩石圈磁场模型及中国磁异常特征的几点认识

介绍了最新的地球磁场模型,包括MF5,NGDC-720和WDMAM。模型MF5是由CHAMP卫星测量得来,它的球谐展开阶次为n=16~100,对应的波长段为400~2500km。模型NGDC-720和WDMAM是综合了卫星磁测、航空磁测、海洋磁测与地面磁测得到数据经过处理后得来,它们有不同的球谐阶次和分辨率。NGDC-720模型是由美国国家地球物理数据中心(The National Geophysical Data Center,NGDC)提供,它的球谐阶次从16阶到720阶,对应于由2500km到56km的波带。M.Purucker博士公布的WDMAM参考模型1是一张分辨率为3′,高度位于WGS84上方5km的磁异常图,它向上延拓后的结果与MF5中的岩石圈磁异常保持一致。作者根据国际上公布的CHAMP、NGDC-720与WDMAM Candidate1的最新数据,绘制了中国及毗邻地区的磁异常图,对中国及毗邻地区明显的大地构造,如造山带,盆地等地区的磁异常特征进行了描述和分析,塔里木、四川、松辽等盆地地区及华北平原部分地区模型中均表现为正异常,西藏高原、天山造山带等地区表现为负异常,而一些深大断裂表现为磁异常高梯度带。通过四川盆地和西藏高原地区三个模型的相互对比,我们发现模型阶次越高,它所反映的磁性体(尤其是浅部地质体)的情况越丰富,不同的是四川盆地的结果随着阶次的增高就越接近航磁结果,而西藏高原随着阶次的增高却和航磁结果差别越来越大。     

Convective mechanism for the formation of photospheric magnetic fields

The well-known model that attributes the formation of a bipolar sunspot group to the emergence of a flux tube disagrees sharply with the usual observed pattern of phenomena. At the same time, the observed patterns can be accounted for quite convincingly in terms of local magnetic-field amplification due to cellular convective motions of the solar plasma. In this study, magnetoconvection in a plane horizontal fluid layer is simulated numerically in the framework of the fully nonlinear, three-dimensional problem. A weak horizontal magnetic field and weak cellular flow are assumed to be present initially. Convection is shown to be capable of producing bipolar magnetic configurations of the strongly amplified magnetic field. Indications of magnetic freezing of the flow in the cell are found. The action of the amplification mechanism under study may be controlled by the large-scale toroidal magnetic field of the Sun.     

Full 3D MHD calculations of accretion flow structure in magnetic cataclysmic variables with strong,complex magnetic fields

We have performed three-dimensional magnetohydrodynamical calculations of stream accretion in cataclysmic variable stars for which the white dwarf primary possesses a strong, complex magnetic field. These calculations were motivated by observations of polars: cataclysmic variables containing white dwarfs with magnetic fields sufficiently strong to prevent the formation of an accretion disk. In this case, an accretion stream flows from the L1 point and impacts directly onto one or more spots on the surface of the white dwarf. Observations indicate that the white dwarfs in some binaries possess complex (non-dipolar) magnetic fields. We performed simulations of ten polars, with the only variable being the azimuthal angle of the secondary with respect to the white dwarf. These calculations are also applicable to asynchronous polars, where the spin period of the white dwarf differs by a few percent from the orbital period. Our results are equivalent to calculating the structure of one asynchronous polar at ten different spin-orbit beat phases. Our models have an aligned dipolar plus quadrupolar magnetic field centered on the whitedwarf primary. We find that, with a sufficiently strong quadrupolar component, an accretion spot arises near the magnetic equator for slightly less than half our simulations, while a polar accretion zone is active for most of the remaining simulations. For two configurations, accretion at a dominant polar region and in an equatorial zone occurs simultaneously. Most polar studies assume that the magnetic field is dipolar, especially for single-pole accretors. We demonstrate that, with the orbital parameters and magnetic-field strengths typical of polars, the accretion flow patterns can vary widely in the case of a complex magnetic field. This may make it difficult formany polars to determine observationally whether the field is pure dipolar or is more complex, but there shoulid be indications for some systems. In particular, a complex magnetic field should be suspected if there is an accretion zone near the white dwarf’s equator (assumed to be in the orbital plane) or if there are two or more accretion regions that cannot be fitted by dipolar magnetic field. Magnetic-field constraints are expected to be substantially stronger for asynchronous polars, with clearer signs of complex field geometry due to changes in the accretion flow structure as a function of azimuthal angle. These indications become clearer in asynchronous polars because each azimuthal angle corresponds to a different spin-orbit beat phase.     

Periodic instabilities in protostellar disks with azimuthal magnetic fields

The stability of magnetohydrodynamic oscillations in a protostellar disk with a toroidal magnetic field is analyzed. It is shown that, apart from the aperiodic magnetorotational instability, two other types of periodic instabilities of non-axisymmetric perturbations can exist. The simultaneous presence of azimuthal and vertical components of the wave vector are necessary for these to exist. One instability is due to the inductive winding-up of the azimuthal magnetic field of the wave, and the other arises when the field amplitude is increased by a comoving Hall wave, transferring magnetic field into a region of enhanced field intensity. The bandwidths of the unstable wave numbers are analyzed as a function of the Hall current, the β parameter of a plasma, and the angle between the direction of wave propagation and the plane of the disk. Regions in the accretion disks typical of T Tauri stars are indentified where these instabilities could be most active.     

Regions of primary energy release of solar flares associated with singularities in the magnetic field

The locations of sites of primary energy release of solar flares are studied. Magnetic singularities revealed earlier—self-intersections (reconnections) of F = 0 surfaces, where F is a differential factor determining the structural singularity in a potential magnetic field—are considered as possible sites of energy release. Six flare events demonstrating paired sources of non-thermal hard X-rays emission observed on March 17, 2002, July 17, 2002, April 6, 2004, November 4, 2004, November 6, 2004, and December 1, 2004 are analyzed for probable singularities. In each event analyzed, each source of non-thermal hard X-rays emission can be associated with an individual magnetic singularity; in other words, there is a magnetic-field line passing near the singularity and ending near (i.e. within about 10″) the source located on the photosphere (in the chromosphere). For the homologous flares observed on November 4 and 6, 2004, the same magnetic singularity is responsible for the source of non-thermal hard X-rays emission observed in the eastern sector of the flare region on November 4 and the source observed in the western part on November 6. A proposed interpretation associates these observations with a reversal of the electric field generated in the magnetic singularity on November 6, compared with the electric field generated on November 4, attributed to corresponding changes occurring in the photospheric magnetic field.     

The phase matrix for scattering in a weak magnetic field. The Hanle effect

A new formulation for the phase matrix for the scattering of radiation in a weak magnetic field is presented. The phase matrix is represented as a product of individual matrices that depend on the angle of incidence and the scattering angle. It is shown that the Hanle effect is absent in observations of scattered light in the solar atmosphere when the magnetic field is perpendicular to the atmosphere. In strong magnetic fields, the phase matrix depends only on the direction of the magnetic field relative to the basic coordinate system.     

A feasibility study simulating superconducting magnetic separators for weakly-magnetic ores

A “straight-wire” flow-through magnetic ore separator has been designed, built, and successfully used to separate magnetite from synthetic slurries. The purpose of these experiments was to simulate the field profile of a “straight-wire” superconducting magnetic separator which would be capable of separating weakly-magnetic hematite ore from typical slurries. Magnetite is used as the test mineral because it experiences the same magnetic forces at low field as does hematite at high field; thereby making possible less expensive low-field simulation.The present separator concept is based on the fact that there is a particle concentration profile due to the gravity field for low-velocity turbulent flow. When an upward magnetic force is applied, the concentration profile of magnetic particles can be reversed leaving the nonmagnetic particles flowing alone at the bottom of the channel. By means of a divider at the end of the channel, the concentrate is separated from the tailings. It is shown that the time needed to deflect hematite particles in a narrow cylindrical channel concentric with the superconducting wire is small enough so that high throughputs in the turbulent flow region are possible. In the case of a high-field superconducting separator, the centrifugal force could replace gravity by rotating the flow around a straight-wire conductor.