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hot plasma
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  热等离子体
    Through solving the radiative transfer equation,we obtain the specific intensity of cyclosynchrotron emission in subrelativistic hot plasma with self absorption.
    对含有磁场的次相对论热等离子体的回旋同步辐射,考虑等离子体的自吸收,求解辐射转移方程,得到等离子体表面向外的回旋同步辐射的辐射强度.
短句来源
    THE CYCLOSYNCHROTRON RADIATION IN SUBRELA TIVISTIC HOT PLASMA WITH SELF ABSORPTION
    次相对论热等离子体中的自吸收回旋同步辐射
短句来源
    Cyclosynchrotron Radiation in Mildly Relativistic Hot Plasma
    次相对论热等离子体中的回旋同步辐射
短句来源
    In solving the radiative transfer equation, we have found the specific intensity of synchrotron emission in relativistic hot plasma with self - absorption.
    对含有磁场的相对论热等离子体的同步加速辐射,考虑等离子体的自吸收,求解辐射转移方程,得到等离子体表面向外的同步加速辐射的辐射强度。
短句来源
    The iron K line can be produced in a variety of X ray illuminated material, and in hot plasma in active galactic nuclei. It provides an important diagnostic of the physical state and the geometry of gas in the active galactic nucleus, as well as the nature of the gravitational potential in the central engine.
    活动星系核中的铁K线辐射可由X射线照射的冷物质 ,热等离子体产生 ,它提供了活动星系核从非常核心到核周围的物质分布 ,物理状态 ,以及中心黑洞强引力场的重要诊断手段。
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  “hot plasma”译为未确定词的双语例句
    (2) The cold and hot plasma were ejected along EUV loops.
    (2)日浪喷发物质沿着EUV环运动.
短句来源
    Ha flare may be caused by heat conduction from 107K-108K hot plasma which generated hard and soft X-ray emissions.
    Hα耀斑主要是由T=10~7—10~8K(产生软硬X射线的热区)等离子体向下传导到色球而形成.
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  hot plasma
This review deals with basic results of experimental and theoretical studies (numerical simulations included) of the distributions, composition, and dynamics of particles of a hot plasma in the geomagnetosphere.
      
The integrity (unity) of the system outer radiation belt-ring current-near plasma sheet is substantiated (the concept of a hot plasma geocorona).
      
Wave resonances in the hydrodynamic model of an isotropic collisionless quasi-neutral hot plasma with isothermal ions and electrons are considered.
      
The Generation of a Dense Hot Plasma by Intense Subpicosecond Laser Pulses
      
The development of a method for studying the features of X-ray emission by multiply charged ions in a dense hot plasma is considered.
      
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Filtergrams of 1B/M1-M4 Ha flare starting at 22h25m of November 11, 1980 are digitized, and isophote lines are drawn in order to compare with hard X-ray, soft X-ray and microwave burst images. The following results are revealed.1. For the first maximum, high energy electrons do not penetrate the chromosphere. Ha flare may be caused by heat conduction from 107K-108K hot plasma which generated hard and soft X-ray emissions.2. The second maximum can be infered to be caused by bremsstralung of high energy...

Filtergrams of 1B/M1-M4 Ha flare starting at 22h25m of November 11, 1980 are digitized, and isophote lines are drawn in order to compare with hard X-ray, soft X-ray and microwave burst images. The following results are revealed.1. For the first maximum, high energy electrons do not penetrate the chromosphere. Ha flare may be caused by heat conduction from 107K-108K hot plasma which generated hard and soft X-ray emissions.2. The second maximum can be infered to be caused by bremsstralung of high energy electrons. The Ha flare maximum occured later than that of X-ray burst for less than 5 seconds.3. During the flash phase the area and the intensity of Ha emission enhanced simultaneously.4. From the changes of transverse magnetic fields outlined by Ha fibrils, 10s' engs magnetic energy is estimated to be released in this flare.

本文对1980年11月5日22点25分开始的1B/M1-M4的Hα耀斑进行了图象处理,绘制了等光度图;与硬、软X射线象,微波象进行了比较.结果表明:1.耀斑的第一次极大,高能电子没有穿透到色球.Hα耀斑主要是由T=10~7—10~8K(产生软硬X射线的热区)等离子体向下传导到色球而形成.2.Hα耀斑的第二次极大,是由高能电子轰击色球而形成,Hα耀斑滞后数秒(小于5秒).3.耀斑闪光相,Hα面积与Hα强度同步增长.4.从耀斑前后的横向磁场变化(Hα短纤维的变化),估计磁能释放~10~(31)尔格.

Observations show that a great deal of thermal elections exist in the rich clusters of galaxies. There is no question but that these thermal electrons interact with the microwave background photons. In this paper, we discuss the distortion of trie microwave background spectrum caused by the thermal electrons in all rich clusters of galaxies. The thermal electrons scatter off the background photons and make the spectrum deviate from the blackbody radiation. In the higher energy region, the distortion is less...

Observations show that a great deal of thermal elections exist in the rich clusters of galaxies. There is no question but that these thermal electrons interact with the microwave background photons. In this paper, we discuss the distortion of trie microwave background spectrum caused by the thermal electrons in all rich clusters of galaxies. The thermal electrons scatter off the background photons and make the spectrum deviate from the blackbody radiation. In the higher energy region, the distortion is less than 1% of the peak intensity of the 2.74 K blackbody radiation and it is agreeable with the observational data of the Cosmic Background Explorer (COBE). Our calculation does not agree with the great distortion (10% of the peak intensity of the 2.74K blackbody radiation) obtained by Matsumoto, et al., The effects on the background radiation from the micro-gravitational lenses by galaxies and from the bremsstrahlung of the hot plasma in the rich clusters of galaxies are too small to be observed

观测表明,富星系团内存在着大量的高温热电子.它们将与微波背景光子相互作用.本文考虑了星系团集合使微波背景辐射产生的畸变.我们的理论估计表明,富星系团集合的高温热电子散射背景光子,使背景辐射谱偏离黑体辐射谱.在背景谱的维恩区,畸变小于2.74K黑体峰值强度的1%,这个结果与最近COBE卫星的探测结果是一致的.没有得到Matsumoto所探测到的在700μm附近有相当于黑体谱峰值强度10%的重大畸变.星系作为微引力透镜,对背景辐射的影响不可能探测得到.星系团内热电子的轫致辐射在微波波段更弱.

In this paper we have calculated the plasma wake fields(PWFs) excited by the interaction of high-energy electron beam with cold and hot plasma, and discussed the effects of electron beam speed, density and its length on PWFs. Based on the obtained results, we have studied τ-profiles of PWFs resulted from the interactions of high energy electron beams produced during a solar impulsive flare with the cororonal plasma, and acceleration of lower energy electrons by this PWFs in the corona. Here τ=ωp(t-x/vb)...

In this paper we have calculated the plasma wake fields(PWFs) excited by the interaction of high-energy electron beam with cold and hot plasma, and discussed the effects of electron beam speed, density and its length on PWFs. Based on the obtained results, we have studied τ-profiles of PWFs resulted from the interactions of high energy electron beams produced during a solar impulsive flare with the cororonal plasma, and acceleration of lower energy electrons by this PWFs in the corona. Here τ=ωp(t-x/vb) where ωp = (4πnoe2/me) and t is time, x the axis along the diraction of electron beam velocity, vb the speed of electron beam, no plasmadensity in the corona, and me the rest mass of electron.

计算了高能脉冲电子束在冷背景和热背景等离子体条件下产生的等离子体尾场(PWF)大小,讨论了高能电子束的速度、密度、长度对等离子体尾场分布的影响.在这基础上,研究了太阳耀斑脉冲相产生的向外逃逸高能脉冲电子束在日冕背景等离子体条件下激发的等离子体尾场分布以及对其捕获电子的加速.

 
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