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plasma pressure
相关语句
  等离子体压力
     There is the condition β<<1 in the tail lobe and β≥1 in the plasma sheet, where β is the ratio of plasma pressure and magnetic pressure.
     尾瓣中满足条件β<<1,而等离子体片中β≥1,其中β为等离子体压力与磁压之比。
短句来源
     The effect of the plasma pressure on the hydrogen content,type of the Si-H bond-ing,photoluminescence,optical gap and the electric transport properties of plasmadeposited hydrogenated amorphous silicon(a-Si:H)has been studied.
     本文主要研究了等离子体压力对射频辉光放电法沉积的非晶硅氢合金(a-Si∶H)膜的组成、结构及性能的影响. 它们包括 a-Si∶H 膜的氢含量、氢的键合形式、光致发光、电导率、光电导、自由载流子寿命及传输机理.
短句来源
     The detached plasma isin a high confinementper formance H mode associated with both a large fraction of edge radiation power(50 %~ 80 % ) and a large drop in plasma pressure along the SOLopen field line (about90 % ) .
     高约束H模状态下的脱靶等离子体沿删削层(SOL)磁力线有大的辐射功率份额(50%~80%)和大的等离子体压力下降(90%)。
短句来源
     Effect of Plasma Pressure on the Properties of a-S∶H Films
     等离子体压力对辉光放电沉积的a-Si:H膜的组成、结构及性能的影响
短句来源
     Simultaneously, the formation mechanism of the following plasma parameters distribution including plasma density, axial current density, plasma velocity, Mach number, ion temperature, electron temperature, ion pressure, plasma pressure and heat flux density to anode was analyzed.
     同时对等离子体密度、轴向电流密度、等离子体速度、马赫数、离子温度、电子温度、离子压力、等离子体压力以及注入阳极的能流密度分布的形成机理进行了分析。
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  等离子体压强
     the electron temperature, Tc= (l9.9?.6) eV, Tw= (20.7?.7) eV. the plasma pressure at 8cm on the right of the west cusp centre is about 6.76Pa, j8^=1.7X10~'.
     东、西会切中心电子温度分别为(19.9±1.6)eV、(20.7±1.7)eV; 距西端会切中心8cm处的等离子体压强约为6.76Pa,β约为1.7×10~(-3);
短句来源
     the plasma pressure at 8cm on the right of the west cusp centre is about 6. 76 Pa, B 1. 7X 10-3. The plasma instability has been observed in the simple mirror, its vibratin frequency was 7-9. 2kHz.
     距西端会切中心8cm处的等离子体压强约为6.76Pa,β约为1.7×10~(-3); 在中心室观测到不稳定性,振荡频率为7~9.2kHz。
短句来源
     THE KELBG POTENTIAL USED IN THE DENSE HYDROGEN PLASMA PRESSURE AT HIGH TEMPERATURE
     KELBG势在高温、稠密氢等离子体压强中的应用(英文)
短句来源
     A boundary theory is used to study the influence of plasma pressure on the coupling behavior of double resistive tearing mode in a multiple current layer.
     应用边界层理论研究了等离子体压强对多层电流片中m≥ 2的双撕裂模耦合的线性和非线性发展行为的影响 .
短句来源
     The results show that the inclusion of the plasma pressure does not change the physical properties of linearly coupled double tearing mode when the plasma β 1. The plasma pressure influences qualitatively the nonlinear evolution tendency of the double tearing mode.
     结果表明 ,当等离子体 β 1时 ,等离子体压强对双撕裂模的两有理面模之间通过撕裂模外区发生耦合作用的线性行为没有定性影响 .
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  “plasma pressure”译为未确定词的双语例句
     It was found that the density of AO varies from -3×l016 to 2×l017 atom/m3 as the plasma pressure was varied from 10-3-10-2 Pa.
     当气压从10-3 Pa-10-2 Pa之间变化时原子氧密度在10 16-10 17/m3之间变化.
短句来源
     The anisotropy of plasma pressure in the magnetosheath has strong influence on the generation of the K-H instability.
     各向异性对K-H不稳定性有显著影响。
短句来源
     It is found from numerical simulation that:the CME triggering model,with a ratio of plasma pressure at its center and that at its edge m≥2,can trigger a CME and can not when m<2.The error for this numerical conclusion is less than 1%.
     当m<2时,上浮CME触发模型不能触发CME,计算结论的误差小于1%.
短句来源
     Study of microscopic drift instabilities in highβ(plasma pressure/magnetic pressure) plasmas is one of advanced topics in plasma theory studies,for it is of great important in understanding the basic plasma behaviors and researching on advanced magnetic confinement fusion and space physics.
     高比压等离子体中的微观漂移不稳定性是等离子体理论研究中的前沿课题之一,它对于理解等离子体的基本行为,对于先进磁约束聚变研究和空间物理研究都有着重要的意义。
短句来源
     Under the assumption that the local plasma pressure gradient is limited by high n ideal MHD ballooning modes,the optimized pressure profile is examined for noncirclar tokamaks.
     本文假定等离子体局部压强梯度由理想磁流体高n气球模所限定,讨论了非圆截面环流器的最佳压强剖面。
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  plasma pressure
This paper discusses the use of Plasma Pressure Compaction to consolidate hafnium diboride powders.
      
Bulk fine-grained copper samples were prepared by consolidating copper powders using the technique of plasma pressure compaction (P2C).
      
Microstructure and hardness of copper powder consolidated by plasma pressure compaction
      
It was found that by lowering the plasma pressure to 50 mTorr near the end of the etch, the organic film can be removed.
      
The plasma pressure has been measured as a function of axial position in the are channel with a Baratron pressure transducer.
      
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The ejection of coronal mass in the form of loop transients was discovered during the skylab, and the white-light coronagraph shows that the outward motion of the coronal transients accelerated or remained at an approximately constont velocity. These loops were like elongated structures. The magnatic energy density for the transient was about 10 times the thermal energy density, indicating that the plasma was magnetically controlled.There are four types of the theoretical models of coronal transients-the purely...

The ejection of coronal mass in the form of loop transients was discovered during the skylab, and the white-light coronagraph shows that the outward motion of the coronal transients accelerated or remained at an approximately constont velocity. These loops were like elongated structures. The magnatic energy density for the transient was about 10 times the thermal energy density, indicating that the plasma was magnetically controlled.There are four types of the theoretical models of coronal transients-the purely hydrodynamical mode, the MHD numerical modeling mode, the ring current mode and the eruptive prominence and transient mode. As to the first two types one problem is that they evoke purely thermal or nonmagnetic driving forces. Since the magnetic energy dominates in these events (β<1), a nonmagnetic driving mechanism is difficult to justify.In the first paper, the Anzer's model is restudied. the equilibrium in the direction of the minor radius of the loop is analysed, and the driving force produced by the plasma pressure is considered. The equation of motion of a section of the coronal loop top and the minimum currpnt of the accelerated motion of the coronal loop are given, and the numerical calculation is completed for the given different initial conditions.In the second paper, we suggest a magnetic loop model, in which the coronal loop is a loop-like magnetic tube of force. The forces driving the coronal loop are produced by the nohhomogeneous distribution of the longitudinal magnetic fields in the magnetic loop. The coronal loop is a slender one.Given the distribution of the longitudinal magnetic fields on the coronal loopBZ=B0r1n, n = 1, 2, 3, ……where B0 is a constant, after analysing the various forces that are exerted on the top fo the coronal loop, one can obtain the equation of motion of the coronal loop top The numerical calculations from Equation ( 1 ) is completed for the given different initiol conditions. The results are compared with those observed during the skylab period from May 1973 to January 1974. The former is largely in accordance with the later.

几年以前天空实验室的观测发现太阳日冕中多数瞬变过程是以环状形式发生质量喷射,并且测得环状瞬变过程前导边缘是加速运动或者是等速运动。这些日冕环是细长的环。环中的磁能密度大约是热能密度的十倍。观测表明:磁场是控制日冕环的主要因素。

The Kelvin- Helmholtz instability at earth's magnetopause is investigated by using CGL approach. Similar to the results obtained in the compressional MHD approximation, the K-H instability can be excited only when vc

The Kelvin- Helmholtz instability at earth's magnetopause is investigated by using CGL approach. Similar to the results obtained in the compressional MHD approximation, the K-H instability can be excited only when vcvu. The anisotropy of plasma pressure in the magnetosheath has strong influence on the generation of the K-H instability. The region close to the subsolar point at the magneto-pause can be unstable even when v0<

本文用无碰撞等离子体的CGL近似,讨论了地球磁层顶的Kelvin-Helmholtz(K-H)不稳定性问题。同可压缩MHD近似一样,CGL等离子体也存在下、上两个临界速度v_c和v_u。不稳定性仅当v_c

In the present paper, the mechanism of magnetospheric substorm which is produced by the energy transportation from the fluctuation kinetic energy of solar wind is extended to the case of collisionless plasma process. The fluctuations of solar wind quantities at the magnetopause excite the compressed Alfven waves, which propagate through the collisionless plasma in the tail of magnetosphere. There is the condition β<<1 in the tail lobe and β≥1 in the plasma sheet, where β is the ratio of plasma pressure...

In the present paper, the mechanism of magnetospheric substorm which is produced by the energy transportation from the fluctuation kinetic energy of solar wind is extended to the case of collisionless plasma process. The fluctuations of solar wind quantities at the magnetopause excite the compressed Alfven waves, which propagate through the collisionless plasma in the tail of magnetosphere. There is the condition β<<1 in the tail lobe and β≥1 in the plasma sheet, where β is the ratio of plasma pressure and magnetic pressure. Hence, the fast magnetosonic waves dissipate very little in the tail lobe and decay rapidly in the plasma sheet, where the wave energies are converted into heat and kinetic energy of the particles. It is shown also that the energy particles in the plasma sheet may be produced by the dissipation o'f the energy from solar wind and are not necessarily originated from the solar wind directly.

本文将太阳风涨落传输能量产生磁层亚暴的机制推广到无碰撞等离子体过程。太阳风的涨落在磁层顶激发压缩阿尔文波,并在磁尾的无碰撞等离子体中传播。尾瓣中满足条件β<<1,而等离子体片中β≥1,其中β为等离子体压力与磁压之比。这样,快磁声波在尾瓣中几乎不衰减,而在等离子体片中很快衰减,将波动能量耗散在等离子体片中使等离子体加热或者粒子加速。这种机制还表明,磁尾等离子体片中的高能粒子可以由太阳风涨落动能耗散而被加速,不一定是直接源于太阳。

 
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