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burst on
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  爆发
     OBSERVATIONS OF MICROWAVE BURST ON 15 APRIL,1998
     1998年4月15日微波爆发观测
短句来源
     Confirmation and Analysis of a Solar Radio Burst on 1993 October 2
     1993年10月2日太阳射电爆发事件的证认和分析
短句来源
     A Preliminary Analysis of A Complex Solar Burst on Sep. 23, 1998 by the Joint Radio Observations
     1998年9月23日复杂太阳爆发射电联合观测的初步分析
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     The Spike-like Structure in A Solare Microwave Burst on May 21,1990
     1990年5月21日微波爆发中的类尖峰辐射结构
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     A Big Complex Microwave Burst——Solar Radio Burst on Oct. 14 in 1980
     一次形态复杂的微波大爆发——1980年10月14日射电爆发
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  “burst on”译为未确定词的双语例句
     The effects of H_2CN_2 treatments to bud burst on advance were the most significant.
     H_2CN_2溶液处理对萌芽期提前效果明显,可提前9~11d。
短句来源
     The Analysis of A Radio Burst on Sept. 8 in 1980
     1980年9月8日射电爆发的分析
短句来源
     Study of a Great Microwave Burst on December 16,1988
     1988年12月16日微波大爆发的研究
短句来源
     The Fast Fine Structure in an Outstanding Solar Radio Burst on Dec.16, 1988
     1988年12月16日太阳射电大爆发的快速精细结构(英文)
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     This kind of "abnormal" phenomenon in the result of the GPS data during the flare burst on November 22,1998 can also be found.
     1998年11月22日耀斑期间的GPS资料计算结果也发现这种异常现象。
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  相似匹配句对
     BURST ANGEL
     来自地狱的天使们 爆裂天使
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     BURST ANALYSIS FOR GSM
     试析GSM中的Burst
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     The prediction of the rock burst
     冲击地压的预测
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     The burst-up of "the clash of civilization
     文明冲突论的破产
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  burst on
Moreover, the fast burst response is achieved with burst on/off time less than 5 ns.
      
Both the Ulysses and Galileo spacecraft detected energetic electrons and Langmuir waves that were associated with a type III radio burst on 10 December 1990.
      
A solar radio burst on 25 August 1999 with fine structures (FS) at 4.5-7.5?GHz is studied in this paper.
      
Characteristics of a type II solar radio burst on 22?March 1998
      
The event is composed of a normal drift type?III burst on the lower frequency side and a reverse drift type III burst appearing almost simultaneously on the high side.
      
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This paper summarizes the analysis f the radio observations of the solar eclipse at wavelengths 3.2, 11.1 and 21 cm in Xinjiang on September 22, 1968 and the main results obtained are: the relation between the flux density of localized source and the activity of the active region on the solar disc, the correlation of the radiation of localized source with the plage and sunspot. According to the analysis of the data of these three wavelengths, we have considered the error analysis of the flux densities of the...

This paper summarizes the analysis f the radio observations of the solar eclipse at wavelengths 3.2, 11.1 and 21 cm in Xinjiang on September 22, 1968 and the main results obtained are: the relation between the flux density of localized source and the activity of the active region on the solar disc, the correlation of the radiation of localized source with the plage and sunspot. According to the analysis of the data of these three wavelengths, we have considered the error analysis of the flux densities of the local radio sources, the angular diameters and heights of these sources, the radio totality, the equivalent radius of the radio sun, and the small burst on the solar disc.

本文综合分析了1968年9月22日新疆日全食3.2、11.1和21厘米波长的射电观测资料,得出了射电源的流量和活动区活动性的关系、射电源辐射与谱斑及黑子的相关等观测结果。另外,从综合三个波段的资料通盘考虑了射电源流量值的误差分析、射电源的角径和高度、射电食甚、射电太阳等效半径和日面小爆发等。

On the basis of past work on hydrodynamic model calculations,in this paper we present the numerical results of the axisymmetric hydrodynamic elasto-plastic model calculation of the contact burst on the surface of sandstone of a one kilo-ton TNT equivalent bomb.The main procedures and preliminary results of the calculation are given;the cratering process and the characteristics of the shock wave in the close-in region and medium ranges are describedf the general picture of the distribution of underground...

On the basis of past work on hydrodynamic model calculations,in this paper we present the numerical results of the axisymmetric hydrodynamic elasto-plastic model calculation of the contact burst on the surface of sandstone of a one kilo-ton TNT equivalent bomb.The main procedures and preliminary results of the calculation are given;the cratering process and the characteristics of the shock wave in the close-in region and medium ranges are describedf the general picture of the distribution of underground stresses,velocities and attenuation curves of the stress components along the symmetric axis are depicted.

在流体模型计算的基础上,我们对一千吨TNT当量的装药在砂岩表面接触爆炸这一问题进行了二维轴对称流体弹塑性模型的数值计算。本文将简要介绍该计算的主要步骤和初步结果,描述了成坑过程和地冲击波的传播规律,给出了下半空间应力和速度的分布图象以及沿对称轴方向各应力分量的衰减曲线。

Spectrum of peak flux of solar type IVdm radio burst is generally characteristic of large spectral index, narrow-band, high flux. In addition decirnetric solar radio burst observed in single frequency records swings with time, period of swings is order of seconds [1, 5].According to [6], it had excluded the possibility that the narrow-band type IVdmsolar radio burst is explained by gyrosynchrotron process. It seems that only plasma emissions would be chosen.We have shown in [7] that spectral character of solar...

Spectrum of peak flux of solar type IVdm radio burst is generally characteristic of large spectral index, narrow-band, high flux. In addition decirnetric solar radio burst observed in single frequency records swings with time, period of swings is order of seconds [1, 5].According to [6], it had excluded the possibility that the narrow-band type IVdmsolar radio burst is explained by gyrosynchrotron process. It seems that only plasma emissions would be chosen.We have shown in [7] that spectral character of solar type IVdm radio burst is explained by mechanism of Langmuir's nonlinear scattering by thermal ion. In this paper, we try to explain character by wave-wave interacting nonlinear process. Our ideas are as follows. The nonthermal electrons accelerated in explosive phase are trapped in coronal mirror, it forms the source of type IVdm radio burst. These nonthermal electrons excite simultaneously low-frequency Whistler wave and high-frequency Lang-muir wave. These two waves' nonlinear coalesce process leads to produce transverse-wave of type IVdm solar radio burst. Available data are taken from [8-10].In this paper, we adopt anisotropic loss-cone gap distribution as distribution function of electrons [11-14]. Energetic part of gap distribution is taken as Gauss's wave packet with central energy of wave packet E=100keV. By means of this, we obtain emissity propagating parallel to magnetic direction and linear growth rate of Whistler indicated in (1) and (2), and that of Langmuir wave in (5)- (6). With these quantity, we may calculate wave number spectral density Wlkl (or Wkww) from solution (9) of wave's radiation transfer equation with t= Ll/vgl (orLw/vgw. The thickness of Langmuir's plasma level Ll is supposed to be Ll-Lw=500km, for example, Pig. 1 describes Wkww diagram of Wpe=2n×500 MHz plasma level. Fig. 2 indicates the diagram of Langmuir's growth rate n at plasma frequency of 2n×200MHz.Coalesce process of Langmuir wave and Whistler wave must satisfy resonance condition Eq. (10). According to [4], under coronal condition, it is not satisfied until that the angle between Langmuir wave Kl and Whistler wave Kw is less than10. Thus. we assume that Kl and KW are parallel to magnetic direction to compute Kw, Kl , Kr by means of linear dispersion relation. Such calculated Langmuir's phase velocity is larger than light velocity. But the phase velocity of Langmuir wave excited by fast electrons is less than light velocity. So Langmuir wave which, is calculated from (5) and (6) can not interact with Whistler wave. However Langmuir wave converts easily into new Langmuir wave due to nonlinear scattering by ion. In this process energy almost conserves, wave number decreases, phase velocity increases. New formed Langmuir wave may interact with Whistler wave. Besides, in scattering process Langmuir wave vector turns toward magnetic field [15]. Hence we can calculate wave number moreover still calculate Langmuir's Wkll by (5) and (6) to replace approximately new Langmuir wave after scattering.Coupling equation of l+ w - t process is Eq. (11). Angular radius of the souree takes 2'.In the corona, because of Qe<burst on Aug. 2, 0330, 1972 (Fig. 3). It is seen from Fig. 3 that spectrum of numerical calculation coincides roughly with that of observation. By comparision with each other, we obtain a nont

本文提议了太阳IV_(dm)型爆发的波-波非线性相互作用机制及其频谱的数值计算方法.假设Iv_(dm)型爆发源位在太阳日冕0.6 R_⊙地方,磁场强度为4G—23G的一个磁瓶.它捕获在爆炸相期间受到加速的非热电子(E_0=100keV).这些各向异性的非热电子同时激发朗谬尔波和哨声波.这两种波的非线性结合过程产生了lV_(dm)型爆发的横波.数值计算1972,8,2,0330的频谱与观测符合较好.两者比较得到非热电子数密度随频率(高度)的分布,还得到IV_(dm)型爆发源中的平均电子数密度为372/cm~3,源中的总的非热电子数为10~(32).这比迥旋-同步加速机制所需的非热电子数少1—2量级.文中还谈到了哨声波调制朗谬尔波导致分米波爆随时间振荡的可能性.

 
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