助手标题  
全文文献 工具书 数字 学术定义 翻译助手 学术趋势 更多
查询帮助
意见反馈
   bursts 在 天文学 分类中 的翻译结果: 查询用时:0.174秒
图标索引 在分类学科中查询
所有学科
天文学
地球物理学
更多类别查询

图标索引 历史查询
 

bursts
相关语句
  爆发
    Characteristics of the Solar Microwave Bursts With Proton Events
    伴随太阳质子事件的微波爆发特征
短句来源
    Statistical Characteristics of Cosmic Gamma-ray Bursts
    宇宙γ射线爆发的统计特征
短句来源
    The Coronal Oscillations Revealed by Solar Hard X-ray Bursts
    太阳硬X射线爆发揭示的日冕振荡
短句来源
    Program Design for Spectral Observations of Type Ⅰ Solar Radio Bursts
    太阳射电Ⅰ型爆发频谱观测和处理程序设计
短句来源
    Observation of Continuously Fast Recording of 10ms Solar Macrowave Bursts at 21cm
    21厘米太阳爆发10毫秒无间隙快速记录观测
短句来源
更多       
  
    Search for 3-10TeV Gamma-ray Bursts Using the Data of the Tibet Ⅱ/HD Air Shower Array
    用羊八井二期/加密阵列数据寻找3~10TeV能区的宇宙伽玛
短句来源
    The Light Curves and the Spectral Harness Ratios of Gamma-Ray Bursts
    Gamma射线的光变曲线和谱硬度比
短句来源
    Dynamics of Intrinsic Pulse and Mechanism of Radiation of Gamma-Ray Bursts
    伽玛内禀脉冲动力学和辐射机制
短句来源
    Gamma-Ray Bursts and Strange Stars
    伽玛射线与奇异星
短句来源
    Progress of the Study of Gamma-ray Bursts(Ⅰ):The Observational Feature and Energy Source
    γ射线的研究进展(Ⅰ):γ的观测特征及能源机制
短句来源
更多       
  “bursts”译为未确定词的双语例句
    THE NONLINEAR SCATTERING MECHANISM OF THE SPECTRUM OF THE TYPE Ⅳ SOLAR DECIMETRIC RADIO BURSTS
    太阳Ⅳ型分米波爆的非线性散射机制
短句来源
    The Development of the High Time Resolution Data Acquisition System of Solar Radio Bursts at 10-cm Wavelength
    波长10厘米太阳射电高时间分辨率数据采集系统的研制
短句来源
    The Ha Characteristics of Hard X-ray Bursts
    硬X射线爆发的Hα特征
短句来源
    Relationship between Sudden Ionospheric Disturbances in D Layer and Solar Microwave Bursts
    电离层D层突然骚扰与太阳耀斑微波射电爆发的关系
短句来源
    The Inverse Compton Scattering in Strong Magnetic Field and the Energy Spectra of Gamma-ray Bursts
    强磁场中的逆Compton散射与γ射线爆能谱
短句来源
更多       
查询“bursts”译词为用户自定义的双语例句

    我想查看译文中含有:的双语例句
例句
为了更好的帮助您理解掌握查询词或其译词在地道英语中的实际用法,我们为您准备了出自英文原文的大量英语例句,供您参考。
  bursts
The protective effect of salicylic acid was manifested as negating the bursts of lectin activity induced by mycoplasma infection.
      
The occurrence of electron bursts does not depend on the geomagnetic disturbance level.
      
Investigation of Long-Wave Radio Bursts from Interball-1 Satellite Observations
      
Long-wave radio bursts recorded on the Interball-1 satellite in the frequency band 100-1500 kHz are analyzed.
      
These bursts were identified with powerful solar flares, during which time fluxes of hard X-ray radiation, meter-wave radio bursts (types II and IV), and coronal transients were observed.
      
更多          


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...

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。

In this paper some characteristics of the solar proton events and proton-active regions during the period 1964 Oct.-1972 Dec.of the 20th cycle are discussed. 1.The frequency distribution of proton events with importance≥1 in 1967— 70 is nearly uniform.In 1971 the proton activity is considerably decreased,but in 1972 it is increased again in coincidence with the sunspot activity. 2.Most of the solar proton events,in particular,the proton events with greater importance,cluster in two preferred time intervals....

In this paper some characteristics of the solar proton events and proton-active regions during the period 1964 Oct.-1972 Dec.of the 20th cycle are discussed. 1.The frequency distribution of proton events with importance≥1 in 1967— 70 is nearly uniform.In 1971 the proton activity is considerably decreased,but in 1972 it is increased again in coincidence with the sunspot activity. 2.Most of the solar proton events,in particular,the proton events with greater importance,cluster in two preferred time intervals. 3.The proton activity is clustered in certain heliographic longitudinal regions. The features of the activity of sunspot and radio-burst are different in different lon- gitudinal regions .For example,in the 60°—90° region,the great majority of proton flares has occurred in large sunspot groups and are associated with cm-outbursts.In the 120°—150° region,on the other hand,most of the proton flares have occurred in small sunspot groups and are associated with weak long-enduring era-bursts. 4.The magnetic configurations of sunspot groups are separated into two classes: normal,having the configurations of ordinary bipolar groups and abnormal,inclu- ding g-configuration,antipolarity,configuration with preceding spot at higher lati- tude and with the magnetic axis inclination greater than 30°.The sunspot groups with abnormal configurations have generated the great majority of the proton flares. 5.The appearance of sources emitted at meter-wavelength over magnetically- complex active regions is favourable to produce proton flares.

本文讨论了第廿周1964.10—1972.12.期间太阳质子活动的一些特点,结果给出:第20周质子活动水平的趋势和黑子活动趋势比较一致,和第19周略有不同;在以约80天为间隔的时间序列上,大多数高级别质子事件集中出现在两个时段上;质子活动有集中在某些经度带的趋势,不同经度带上的黑子活动和质子耀斑伴生的射电爆发等具体特点有比较明显的差别;按磁结构将黑子群分成正常和“异常”两类,具有“异常”磁结构的黑子群产生大部分质子耀斑;复杂磁结构的活动区上米波源的出现有利于产生质子耀斑.

This paper consists of three parts. In the first part the 16-dish E-W interferometer of the Mi-Yun Station,Pe- king Observatory(working frequency 146 MHZ)is decribed.Measured instrumental parameters are compared with theoretical ones.Thus the measured beamwidth was 5′.4(5′.3 theoretical),the first sidelobe level amounted to 5%(4.5% theoretical)and the locations of grating lobes in the celestial sphere were very close to the theoretical positions.These show that the surveying of baseline,the installation of antennas...

This paper consists of three parts. In the first part the 16-dish E-W interferometer of the Mi-Yun Station,Pe- king Observatory(working frequency 146 MHZ)is decribed.Measured instrumental parameters are compared with theoretical ones.Thus the measured beamwidth was 5′.4(5′.3 theoretical),the first sidelobe level amounted to 5%(4.5% theoretical)and the locations of grating lobes in the celestial sphere were very close to the theoretical positions.These show that the surveying of baseline,the installation of antennas and the adjustment of transmission lines are reasonably accurate in our case. The observations of the quiet sun and the slowly varying component are described in the second part.In contrast to the results obtained by some authors(e.g.by O'Ob- rien),we found that the apparent diameter of the meter-wave sun had not varied during the descending phase of the solar cycle. In the third part of this paper the results of measurements of type-Ⅰ sources are analyzed.According to the rate of occurence of type-Ⅰ bursts,the sources are classified into four classes.It is found that(1),the average height above photosphere of so- urces of all classes as measured at the central region of the solar disc was 0.24-R_⊙;(2), the E-W distribution of sources was asymmetric with respect to the solar meridian,in agreement with the result of Fokker;(3),the frequency distributions over the solar disc were different for sources of different classes.The sources containing more type- I bursts decreased more rapidly than the continuum sources with respect to the height;(4),the correlation between the commencement of noise storms with the appearance of optical flares seemed to be rather weak.This differed from the result of Mallinge; and(5),the occurence of noise storm sources was closely connected with the mean flare index of the plage region.As shown in fig.10,for all plage regions asso- ciated with large sunspots and strong magnetic fields,the mean flare index had an average value of 14.33(light solid line,fig.10),among these regions for those also containing meterwave sources,this value rose up to 27.15(heavy solid line,fig.10), while for those which did not possess meter-wave sources,the average index was 7.32 (Chain line).

全文分三部分:第一部分描述了北京天文台密云工作站的东-西16面天线干涉仪系统(工作频率146兆赫),并将仪器参数的实测结果与理论予期值相比较.第一旁瓣5%,瓣宽5.4.方向瓣在天球上的位置也都与理论预期相差不大.第二部分描述了宁静太阳及其缓变成分的观测.在太阳活动下降期没有发现米波太阳视直径的变化.第三部分分析了 I 型源的观测结果.米波源的高度我们测定在过日心径时为光球之上0.24R☉.检查不同类型噪暴源按日心径的分布,得出随着高度的增加 I 型源的噪暴成分比起连续的增强辐射下降得要迅速.在与光学现象的对应上,噪暴的起始似乎与耀斑的发生的相关性不强.噪暴源却与谱斑区的平均耀斑指数有密切关系.

 
<< 更多相关文摘    
图标索引 相关查询

 


 
CNKI小工具
在英文学术搜索中查有关bursts的内容
在知识搜索中查有关bursts的内容
在数字搜索中查有关bursts的内容
在概念知识元中查有关bursts的内容
在学术趋势中查有关bursts的内容
 
 

CNKI主页设CNKI翻译助手为主页 | 收藏CNKI翻译助手 | 广告服务 | 英文学术搜索
版权图标  2008 CNKI-中国知网
京ICP证040431号 互联网出版许可证 新出网证(京)字008号
北京市公安局海淀分局 备案号:110 1081725
版权图标 2008中国知网(cnki) 中国学术期刊(光盘版)电子杂志社