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flare
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  耀斑
    ANALYSIS OF H_α PROFILE OF THE LARGE SOLAR FLARE ON JULY 10, 1959
    1959年7月10日太阳特大耀斑的H_α光谱分析
短句来源
    THE STELLAR "FLARE" MODEL FOR COSMIC γ-RAY BURST
    宇宙γ射线爆的恒星“耀斑”模型
短句来源
    A PRELIMINARY ANALYSIS OF THE DOUBLE-RIBBON FLARE OF 23 JULY 1980
    1980年7月23日3B级双带耀斑
短句来源
    Sunspot Group No. 184 in April 1980 and the Flare on April 7 in 1980
    1980年4月份184号黑子群及4月7日耀斑
短句来源
    The Large Flare on July 14 in 1980 and the Velocity Field
    1980年7月14日太阳大耀斑和速度场
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  闪光
    Usually a part of the flare is ejected to distances ranging from 2×10~4 km to 2.5×10~5 km above the base of the chromosphere.
    边缘耀斑的光度和定位测量得出下列结果:(1)在耀斑的闪光阶段存在着剧烈的径向物质抛射,常常耀斑的一部分被抛射到色球层之上高达2·10~4公里到2.5·10~5公里处.
短句来源
    (4)During the flash-phase of the flare the velocity of ejection varies directly with the rate of increase of brightness.
    (4)在耀斑闪光阶段,抛射速度直接地随亮度增加的速率而变化.
短句来源
    The main results are:1.The locations of initial brightening and the characteristics of morphological evolution of the major flare on 4 Feb., 1986 have a close correlation to the newly emerging electric current/magnetic loop system flowing along the northsouth neutral (H11 = 0) line.
    主要结果是: 1.4日大耀斑的初始亮点和闪光相的主要形态演化,与活动区中沿中性线新浮现的强大电流/磁环系密切相关。
短句来源
  耀发
    The present review is given of stellar flares in classical flare stars as well as the RS CVn binary stars.
    本文对经典耀星和RS CVn型双星中的耀发现象作了综述。
短句来源
    It is argued by many researchers that the stellar flare is something similar to solar white flare and its optical radiation is of quasi-black-body and from deep chromosphere with limited emission area.
    许多研究者认为,恒星的耀发类似于太阳白光耀发,它的光学辐射是类黑体的,来自较深的色球层和一定的耀发面积。
短句来源
    It was identified as BD+47 819, near the open cluster α Per. From its spectroscopicly observational result, we can confirm that it is an A5 type star. Its nature is very different from the traditional theory of stellar flare.
    本文作者在对αPer疏散星团的观测工作中发现了一颗罕见的早型亮耀星,从对其光谱观测的结果,可以确定它为-A5型星.这与传统恒星耀发理论是相悖的。
短句来源
    GRB 970508 shows complex behaviour in optical bands, its red shift has been determined to be 0.835 ≤ z ≤ 2.1, and a radio flare was observed about five days after the burst.
    GRB970508的光学余辉有较为复杂的表现,并测出其红移范围0.85<z<2.1。 在该暴发生约五、六天之后,还观测到了射电耀发现象。
短句来源
    It is the first time that the spectra of the core of 3C273 and a new component, which caused the flux flare of 3C273 at the beginning of 1988, were obtained. Also, it is scientific basics for a new model used to explain the phenomena happened in 3C273.
    我们首次获得3C273的“核”和产生流量耀发的新子源的频谱,它为我们提出新的解释模型提供了物理依据。
短句来源
  “flare”译为未确定词的双语例句
    Quasi-Periodic Pulsition and the Elementary Flare Bursts of the Radio Spike Event of August 17,1989
    1989年8月17日太阳射电尖峰事件的准周期脉动及EFB分析
短句来源
    BD+47819: an A5 Type Peculiar Flare Star
    BD+47819:一颗A5型特殊耀星
短句来源
    The X-Ray Emission From A dMe Flare Star
    dMe耀星的X射线的辐射
短句来源
    Correlation between TeV γ ray Flare and Hard X ray Burst in Mrk 421
    Mrk421中TeV和X射线爆发的相关性
短句来源
    4. The off-band obecrvations show that there exists the descending motion of material during the eruption of the flare.
    4.离带观测表明存在着物质的下降运动。
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  flare
Solar Flare Peculiarities: A Hypothesis for a New Phenomenological Model
      
An intensity time-profile of the hard X-ray emission in two cores of a small impulsive solar flare is analyzed.
      
The instant of long-wave radio burst generation seems to correspond to the expansion phase of a flare.
      
It is shown that the spectra and decay times of both protons and electrons are approximately invariant relative to the flare coordinates in a wide angular range.
      
The classifications of magnetic storms by the Kp and Dst indices, the solar flare classifications by optical and X-ray observations, and the classifications of different geoeffective interplanetary events are compared and discussed.
      
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De brusques sursauts lumineux s'observent sur de nombreux types stellaires, notamment les naines rouges proches du Soleil (type UV Ceti) et les étoiles appartenant à une association (type T Tauri). On donne d'abord la liste de 20 étoiles UV Ceti certaines (tableau 1), puis on étudie les variations lumineuses: amplitude des sursauts, courbes de lumière (tableau 2); rapidité des flares, pouvant atteindre 0.25 mag/sec lors de la montée au maximum; fréquence des sursauts. On examine ensuite les variations...

De brusques sursauts lumineux s'observent sur de nombreux types stellaires, notamment les naines rouges proches du Soleil (type UV Ceti) et les étoiles appartenant à une association (type T Tauri). On donne d'abord la liste de 20 étoiles UV Ceti certaines (tableau 1), puis on étudie les variations lumineuses: amplitude des sursauts, courbes de lumière (tableau 2); rapidité des flares, pouvant atteindre 0.25 mag/sec lors de la montée au maximum; fréquence des sursauts. On examine ensuite les variations en dehors des flares (tableau 3). Le spectre présente toujours de l'émission (H et Ca Ⅱ); lors des sursauts on remarque le renforcement du fond continu et l'apparition de HeⅠ et HeⅡ, montrant une forte élévation de température, mais qui n'intéress qu'une petite portion de la surface de l'étoile (1 à 3%). Les UV Ceti sont des étoiles de très faible luminosité (M_(pg) 13) mais très nombreuses; elles appartiennent à la population Ⅰ. On rappelle ensuite la découverte des variations rapides de plusieurs étoiles du type RW Aurigae, et l'on examine les decouvertes d'étoiles à sursauts faites dans la zone du Taureau (tableau 5) la nébuleuse d'Orion (tableau 6) et NGC 2264 (tableau 7). On étudie ensuite les variations lumineuses, et surtout les relations existant entre les UV Ceti et les T Tauri: courbe de lumière, type spectral, appartenance à la population Ⅰ. On discute certains points (différences de luminosité absolue, de spectre, position sur le diagramme H-R). En conclusion les UV Ceti et les T Tauri forment un groupe; les différences observées entre les deux types ont sans doute pour origine a la fois la "sélection observationnelle" et une différence réelle dans le degré d'évolution des étoiles.

我们在有些恒星上观测到它们的光亮骤然发生变化,例如和太阳隣近的红矮星(鲸鱼UV型)和属於某一星協的星(金牛T型). 本文先列出20颗确定为鲸鱼UV型的星(表1),然後讨论它们的光变情况,如躍变的幅度,光变曲线(表2),闪光的速度(在上昇到极亮时,速度可达0.25星等/秒),躍变的频率等.跟着我们更讨论这些星不在闪光的时候的变化(表3). 这些星的光谱内常有发射线(H与CaⅡ),闪光的时候,光谱上的连续背景加强,并且出现HeⅠ和HeⅡ的谱线,表示温度增加很高,但是这仅限於星的很小的表皮层(1至3%). 鲸鱼UV型星自身亮度很弱(M_(pg)13),数目很多,属星族Ⅰ. 本文内提到几颗御夫RW型星的迅速变化,并且讨论了金牛区(表5),猎户星雲区(表6)和NGC2264里(表7)的闪光星. 我们研究了光变的情况,特别说明鲸鱼UV型星和金牛T型星之间的关系:例如在光曲线、光谱型和同属星族Ⅰ几个方面.我们也讨论了这两型星在绝对星等、光谱和赫-罗图上的位置三者的差异. 最後我们断定鲸鱼UV型星和金牛T型星实在是相同的一群;我们由观测得到的它们之间的差异,其原因一则由於“观测上的选择性”,再则由於这两型星的演化阶段有所不同...

我们在有些恒星上观测到它们的光亮骤然发生变化,例如和太阳隣近的红矮星(鲸鱼UV型)和属於某一星協的星(金牛T型). 本文先列出20颗确定为鲸鱼UV型的星(表1),然後讨论它们的光变情况,如躍变的幅度,光变曲线(表2),闪光的速度(在上昇到极亮时,速度可达0.25星等/秒),躍变的频率等.跟着我们更讨论这些星不在闪光的时候的变化(表3). 这些星的光谱内常有发射线(H与CaⅡ),闪光的时候,光谱上的连续背景加强,并且出现HeⅠ和HeⅡ的谱线,表示温度增加很高,但是这仅限於星的很小的表皮层(1至3%). 鲸鱼UV型星自身亮度很弱(M_(pg)13),数目很多,属星族Ⅰ. 本文内提到几颗御夫RW型星的迅速变化,并且讨论了金牛区(表5),猎户星雲区(表6)和NGC2264里(表7)的闪光星. 我们研究了光变的情况,特别说明鲸鱼UV型星和金牛T型星之间的关系:例如在光曲线、光谱型和同属星族Ⅰ几个方面.我们也讨论了这两型星在绝对星等、光谱和赫-罗图上的位置三者的差异. 最後我们断定鲸鱼UV型星和金牛T型星实在是相同的一群;我们由观测得到的它们之间的差异,其原因一则由於“观测上的选择性”,再则由於这两型星的演化阶段有所不同. 许多恒星的光亮表现突然的增加,或者说很迅速地发出“闪光”,在几分钟、有时在几秒钟内,星光有显著的增加,跟着变暗,初迅速而渐缓慢. 这种星光的躍变在许多型星都观测到,特别是在绝对亮度微弱的星上面.我们现在只讨论下列的主要两类恒星:

From a large number of H_a photographs of limb flares,fifteen have been selected for reduction.The films were obtained with the standard Lyot-type Chromospheric patrol telescope at the Purple Mountain Observatory during the years 1959—1960. The photometric and positional measurements of limb flares have led to the following conclusions: (1)There are violent radial ejections of matter during the flash-phase of the flare. Usually a part of the flare is ejected to distances ranging from...

From a large number of H_a photographs of limb flares,fifteen have been selected for reduction.The films were obtained with the standard Lyot-type Chromospheric patrol telescope at the Purple Mountain Observatory during the years 1959—1960. The photometric and positional measurements of limb flares have led to the following conclusions: (1)There are violent radial ejections of matter during the flash-phase of the flare. Usually a part of the flare is ejected to distances ranging from 2×10~4 km to 2.5×10~5 km above the base of the chromosphere. (2)The mean velocity of ejection is of the order of 30 km/sec—400 km/sec.The maximum velocity appears in the initial stage of ejection and decreases later on.The acceleration of ejection is supergravitational. (3)The ejective motions of flares are regular and apparently connected with the magnetic fields of the active regions. (4)During the flash-phase of the flare the velocity of ejection varies directly with the rate of increase of brightness. In conclusion,it is noted that the appearance of radio events is closely related to the ejection.

在大量的 H_α边缘耀斑电影胶卷中,为了精炼起见我们选取了15套.电影胶卷是在1959年—1960年期间用紫金山天文台的利奥型色球望远镜拍摄的.边缘耀斑的光度和定位测量得出下列结果:(1)在耀斑的闪光阶段存在着剧烈的径向物质抛射,常常耀斑的一部分被抛射到色球层之上高达2·10~4公里到2.5·10~5公里处.(2)抛射的平均速度是30公里/秒—400公里/秒的数量级,最大的速度出现在抛射的初始阶段,抛射的加速度是超引力的.(3)耀斑的抛射运动是有规则的,且明显地与活动区的磁场有关.(4)在耀斑闪光阶段,抛射速度直接地随亮度增加的速率而变化.最后,注意到了射电事件的出现与抛射密切有关.

141 typical magnetic storms of the sudden commencement (SC) type, of which 45, 42 and 54 have strong, weak and no main phase respectively, have been selected from the magnetographs obtained at Zo-Se observatory during 1936~1962. Using data of solar flares and radio bursts of type 1V, the flares corresponding to the storms have been identified. The statistical properties of the three types of storms and their corresponding flares are investigated by statistical mathod. The charecteristics of...

141 typical magnetic storms of the sudden commencement (SC) type, of which 45, 42 and 54 have strong, weak and no main phase respectively, have been selected from the magnetographs obtained at Zo-Se observatory during 1936~1962. Using data of solar flares and radio bursts of type 1V, the flares corresponding to the storms have been identified. The statistical properties of the three types of storms and their corresponding flares are investigated by statistical mathod. The charecteristics of corpuscular streams emitted by flares are evaluated. By means of correlation analysis, the relations between storm's charecteristics and the charecteristics of flares as well of corpuscular streams are investigated. The main conclusions are as follows; 1. The flares producing the storms with strong main phase are stronger. They concentrate mainly near the central meridian of the solar disk; while the flares producing the storms with weak or no main phase are weaker. The distribution on the solar disk of the former have strong east-west asymmetry, while that of the latter are rather uniform. 2. The formation of the storm's main phase is closely related to the velocity of the corpuscular stream, while the relation with the density of stream, is poor. On the average, the density at the front of streams producing SC storms is 10~40 proton/cm~3. 3. The emitting angle of the corpuscular streams producing SC storms is about 120°±(20°~30°). The lower limit of the total kinetical energy of streams is 10~(27)~10~(28)erg. 4. a_(p max) and K_(p max)—maximum values of α_p and K_p during storms- are closely correlated with the velocity v of streams, while the correlation between the maximum amplitude ΔH_(max) of storm's main phase and v is very poor. 5. The geomagnetic latitude of the Sun, i. e that of subsolar point, affects not only the type, but also the intensity of storms, and it appears that the effect on intensity is more inportent.

根据1936—1962年佘山地磁台磁照图,选出141个典型的急始型(SC)磁暴,其中强主相、弱主相和无主相磁暴分别为45个、42个、54个。利用耀斑和1V型射电暴等资料证认出对应的耀斑。用统计方法研究了三类磁暴及对应耀斑的统计特性。估计了耀斑抛射的微粒流的特性。用相关分析研究了磁暴特性同耀斑和微粒流特性的关系。本文得到的主要结论是: 1.产生强主相SC磁暴的耀斑较强,主要集中在日面中心经圈附近;产生弱主相和无主相SC磁暴的耀斑较弱,前者沿日面的分布有明显的东西不对称性,后者沿日面的分布比较均匀。 2.磁暴主相的形成同微粒流的速度关系密切,但同微粒流密度的关系不大。平均而言,SC磁暴对应微粒流前锋处的密度是10—40质子/厘米~3。 3.SC磁暴对应微粒流的抛射角约为120°±(20°—30°),总动能的下限为10~(27)—10~(28)尔格。 4.磁暴时ap和Kp的极大值ap_(max)和Kp_(max)同微粒流速度v关系密切,而磁暴主相极大振幅ΔH_(max)同v的关系却很不密切。 5.太阳的磁赤纬(卽日下点的地磁纬度)对磁暴的强弱和类型都有影响,可能主要影响强弱。

 
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