吴堡矿区横沟井田矿井充水因素评价     

杨智国  梁秀娟 《陕西地质》2007,35(1):78-83

吴堡矿区赋存着丰富的煤炭资源,但开采技术条件较复杂,其中水文地质条件复杂是影响煤炭开采的主要不利开采技术条件。本文依据横沟井田勘探资料,较全面地分析了井田水文地质条件,并着重评价了井田矿井充水因素。认为黄河水对横沟井田煤炭开采无影响;奥灰承压水对山西组煤层开采在正常地段不会造成危害,对太原组煤层开采有很大的威胁。并提出太原组煤层能否开采利用,还需进一步作详细地质勘查研究工作。  相似文献   

北太平洋风暴轴异常变化特征及其与纬向风场的关系研究   总被引：7，自引：2，他引：7       下载免费PDF全文

韩博  任雪娟  杨修群 《气象科学》2007,27(3):237-245

摘要本文通过对300 hPa5、00 hPa和850 hPa的北太平洋风暴轴(PST)的异常研究,分别提取出两个主异常模态进行比较。分析表明在三层的第一主模态都主要对应有PST异常的准10 a的周期变化;而对300 hPa和500 hPa的第二主模态,以及850 hPa的第三模态,对应有更长时间的趋势变化。进一步通过相关的分析,说明PST的异常从低层到高层的变化存在一定的一致性。通过PST与纬向风场在300 hPa的相关分析发现,两个模态与纬向风场的异常在空间上都呈同位相的分布,说明高层纬向风场异常与PST发展可能存在一种互相反馈的作用。进一步通过斜压增长率和水平两维的E-P通量矢的合成分析发现,这种反馈作用,无论从纬向风场异常所产生的环境斜压增长条件的改变,还是从平均动能与扰动动能的转化关系,都是存在的。  相似文献   

Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity     

C. G. Campbell  & P. M. Heptinstall 《Monthly notices of the Royal Astronomical Society》1998,301(2):558-568

A full numerical solution is found for the effect of a strongly magnetic star on its accretion disc, for the case of magnetic buoyancy diffusion. As in the previously considered case of turbulent diffusion, the disc becomes disrupted when magnetic and viscous stresses become comparable. A magnetically induced temperature elevation leads to electron scattering opacity and radiation pressure becoming significant far from the stellar surface, with consequent viscous instability and vertical disruption of the disc. This, together with the previous turbulent case, suggests that such a disruption mechanism owing to strongly magnetic accretors is generally operable.  相似文献   

Spectroscopic observations of the eclipsing polar MN Hya (RX J0929–24)     

Gavin Ramsay  & Peter J. Wheatley 《Monthly notices of the Royal Astronomical Society》1998,301(1):95-100

We present low–medium resolution optical spectroscopy of the eclipsing AM Her system MN Hya (RX J0929–24). We determine the magnetic field strength at the primary accretion region of the white dwarf to be 42 MG from the spacing of cyclotron features visible during π ∼ 0.4–0.7. From spectra taken during the eclipse we find that the secondary has an M3–4 spectral type. Combined with the eclipse photometry of Sekiguchi, Nakada &38; Bassett and an estimate of the interstellar extinction we find a distance of ∼300–700 pc. We find unusual line variations at π ∼ 0.9: Hα is seen in absorption and emission. This is at the same point in the orbital phase at which a prominent absorption dip is seen in soft X-rays.  相似文献   

PSR J1012+5307: younger than it looks?     

L. Burderi  A. R. King  & G. A. Wynn 《Monthly notices of the Royal Astronomical Society》1998,300(4):1127-1130

Lorimer et al. have recently reported that the spin-down age (∼7 × 10⁹ yr) of the low-mass binary pulsar PSR J1012+5307 is much higher than the cooling age (3 × 10⁸ yr) of its white dwarf companion. The proposed solutions for this discrepancy are outlined and discussed. In particular, the revised cooling age estimate proposed by Alberts et al. agrees with data from other low-mass binary pulsar systems if a transition to the 'classical' cooling regime occurs between ∼0.14 and ∼0.28 M_⊙. If this transition is excluded, PSR J1012+5307 seems to have finished its accretion phase far from the spin-up line.  相似文献   

Study on the fractal character of magnetic anomaly fields and the delineation of tectonic elements in the South China Sea     

姜效典  于增慧 《中国海洋湖沼学报》1998,16(1):28-35

INTRODUCTION~hon0ffornjcelmtSwnthebasisofthestudyonthecrustaldefonnationanddeVel0prnent,thedistributionofndnereIs,andthendnerogeneticlawr.ThegeornagneticfieklisthecomP0siterefledionoftheformati0nanddefortnationofthecrust.Sornagnct-icsLLrVeydatacomPriseirnPortantbasisfordelincatingthearchiteCtonicelements,dCtendningtheirboundarylines,andanalopngthesanndarystrudriineachelernent,whicharetthernaintasks0fgoophySicalworkers.Thegoornagneticdelineati0nofanareahadforlongbodonequalitativeybyobs…  相似文献   

Measurements of the direction of the solar wind using interplanetary scintillation     

P. J. Moran  A. R. Breen  C. A. Varley  P. J. S. Williams  W. P. Wilkinson  J. Markkanen 《Annales Geophysicae》1998,16(10):1259-1264

EISCAT observations of the interplanetary scintillation of a single source were made over an extended period of time, during which the orientation of the baselines between the two observing sites changed significantly. Assuming that maximum correlation between the scintillations observed at the two sites occurs when the projected baseline is parallel to the direction of plasma flow, this technique can be used to make a unique determination of the direction of the solar wind. In the past it has usually been assumed that the plasma flow is radial, but measurements of eleven sources using this technique have indicated conclusively that in at least six cases observed at mid or high heliocentric latitude there is a significant non-radial component directed in four cases towards the heliocentric equator and in two cases towards the pole.  相似文献   

IMP 8 magnetosheath field comparisons with models     

Z. Kaymaz 《Annales Geophysicae》1998,16(4):376-387

This study presents cross-sectional vector maps of the magnetic field derived from IMP 8 magnetometer in the magnetosheath at 30 R_e behind the Earth. In addition the vector patterns of the magnetosheath field for northward, southward, and east-west interplanetary magnetic field (IMF) directions are qualitatively compared with those obtained from the Spreiter-Stahara gas dynamic (GD) and Fedder-Lyon magnetohydrodynamic models (MHD). The main purpose is to display the cross-sectional differences in relation to the dayside merging with different IMF directions, allowing the reader to make direct visual comparisons of the vector patterns. It is seen that for east-west IMF directions, the data-based and MHD-based patterns differ noticeably in a similar way from the GD model, presumably reflecting the influence of dayside magnetic merging of the Earths magnetic field with the y-component of the interplanetary magnetic field. All three northward IMF cross sections show comparable field draping patterns as expected for a closed magnetosphere. For southward IMF case, on the other hand, differences between the three cross-sectional patterns are greater as seen in the field vector sizes and directions, especially closer to the magnetopause where more disturbed magneto-spheric conditions are known to be exist. The data comparisons with the MHD and GD models show that the differences result from the magnetic field-flow coupling and that the effects of dayside reconnection are present in IMP 8 magnetic field measurements.  相似文献   

Velocity of auroral arcs drifting equatorward from the polar cap     

P. J. S. Williams  C. F. del Pozo  I. Hiscock  R. Fallows 《Annales Geophysicae》1998,16(10):1322-1331

The drift velocity of an auroral arc is compared with the component of F-region plasma velocity in the same direction for ten cases where the arc is seen to move steadily equatorward for several minutes without any major change in appearance or orientation. In most cases the two velocities are close, but on two occasions the drift velocity of the arc is much higher than the plasma velocity. From the cases studied it appears that during the growth and recovery phase of the substorm cycle the arc moves with a velocity close to the convection velocity, but during the expansion phase this is not the case.  相似文献   

Evolution of Magnetic Fields in Galaxies with Spiral Structure     

Rohde  R.  Elstner  D.  Rüdiger  G. 《Studia Geophysica et Geodaetica》1998,42(3):382-390

We present simulations of the 3D nonlinear induction equation in order to investigate the temporal evolution of large-scale magnetic fields in spiral galaxies. Our model includes differential rotation, ambipolar diffusion and, based on small-scale turbulence, eddy diffusivity and the tensorial -effect with magnetic feedback. The nonaxisymmetric spiral pattern and – if considered – the vertical stratification of the galaxy are represented in its density and turbulence profile. Neglecting vertical stratification the lifetime and geometry of an initial magnetic field depend on the correlation time of interstellar turbulence _corr . Short correlation times increase the lifetime of the initial magnetic field, but the field is rapidly wound up. Its pitch-angles develop to zero. The magnetic field has disappeared after at most 1 to 1.5 Gyr. A resonance like phenomenon is found by tuning the pattern velocity of the galactic spiral. The simulations then show an exceptional amplification of the magnetic field in the case that the pattern speed and a magnetic drift velocity have similar values. Considering a vertical stratification we achieve sufficiently long living grand-designed magnetic fields excited by dynamo action. The behaviour and geometry of the resulting field is again significantly influenced by the correlation time _corr . Small values of _corr lead to axisymmetric fields with small pitch-angles and field-concentration between the spiral arms. Increasing the correlation time the solutions show larger pitch-angles; and depending on very large correlation times the galactic dynamo rather generates fields clearly within the spiral arms and having a bisymmetric structure.  相似文献