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      april
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  4月
    The Influnce of the solar eclipse on 19 April 1958 on the Ionosphere at Wuhan
    1958年4月19日武昌地区日食对电离层的影响
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    MAXIMA OF THE BRIGHTNESS AND AREAS OF SOLAR H_α FLOCCULI IN JANUARY—APRIL 1971 AND THEIR CORRELATIONS WITH FLARES
    1971年1—4月太阳H_α谱斑亮度、面积的极大同耀斑的相关性
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    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
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    The Motion of the Flare Loop prominence On April 27 in 1981
    1981年4月27日的耀斑环珥运动
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    Hα Observation of the Great Eruptive Loop-Prominence on the Western Limb on April 27 in 1981
    1981年4月27日日面西边缘大爆发环珥事件的H_α观测
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  四月
    On the Record in the Night of April 5, 687B.C.: Stars were not Seen and Stars Fell Like Rain at Midnight
    论鲁庄公七年夏四月辛卯夜,恒星不见,夜中星陨如雨
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  “april”译为未确定词的双语例句
    In this paper, we analyse one photoelectric record of the occultation of SAO150330 by Comet P/Crommelin on the night of 1 April, 1984. There are two secondary occultations around the main one, which were probably caused by two jets.
    本文对1984.4.1夜P/Crommelin彗星掩恒星SAO 150330的光电观测记录进行了分析,发现该彗星除了主掩外还有两个次掩(可能是由两股喷流所致),估算后,得到如下结果: 两个喷流宽度均为72.8 km左右;
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    MORPHOLOGICAL FEATURES OF A LARGE SOLAR ACTIVE REGION FROM APRIL TO MAY IN 1978
    1978年4—5月太阳大活动区的形态特征
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    THE MAGNETIC FIELD AND FLARES OF GREAT SUNSPOT GROOP IN LATE APRIL, 1978
    1978年4月底大黑子群的磁场和耀斑
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    A Sunspot Group Which Rapidly Emerged on April 5 in 1980
    1980年4月一个快速浮现的黑子群
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    THE MAGNETIC FIELD AND FLARES OF GREAT SUNSPOT GROUP IN LATE APRIL 1978
    1978年4月底大黑子群的磁场和耀斑
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  april
       While the EAB emergence period ranged from mid May to late May in 2003, it ranged from mid April to mid May in 2004 (in laboratory).
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       From April to July 2003 and 2004, we surveyed the nest-site selection of the White Eared pheasant (Crossoptilon crossoptilon) in the Zhujie Monastery and in the mountain facing it in Sichuan Province, China.
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       The precipitation, runoff, and normalized difference vegetation index (NDVI) data of six catchments were accumulated from April to September in 1992, 1993, and 1995.
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       The feeding habitat selection of blue sheep (Pseudois nayaur) was studied by direct observation method in the Helan Mountains, China during winter (from November to December) and spring (from April to June) from 2003 to 2004.
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       canadensis lasts from March to October, with a peak from April to May.
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         In this paper the ionospheric data during the solar eclipse on 19 april 1958 at Wuhan is analyzed.Changes of the electron density and recombina- tion coefficient of E-layer and radiation source have also been discussed.
            本文作者利用1958年4月19日在武汉日食时的电离层观测资料,计算了电子数密度的变化和 E 层的复合系数,且也讨论了 F_2层的反常和幅射源的分布。
文摘来源
         Photometric observations of Nova Her 1963 were started in Peking on Feb.18, 1963,with a photoelectric photometer mounted on a 15 cm aluminized Cassegrain reflec- tor.The Nova was observed in the ultraviolet,blue,yellow,and red as well as through four relatively narrow-band filters whose commercial type designations being S43,S47, S50 and S53,with maximum transmissions of the cell-field lens-filter combination at about 4300,4550,4850 and 5230(?) respectively. Table 1 lists the types and parameters of the fil...
            北京天文台筹备处自制了一架光电光度计,在1963年2月到6月间进行了对1963年武仙座新星的光电观测.所用的波段,宽波段滤光片是 UG1、GG13、BG12、GG11和 RG1,窄波段是 S43、S47、S50和 S53.
文摘来源
         The following model has been suggested for cosmic γ-ray burst: Cosmic γ-ray burst is an event analogous to solar flare, but much more drastic in scale; the magnetic energy stored in stellar "flare" is converted into kinetic energy of electrons during burst; a great number of relativistic electrons rush out from stellar "flare" within a very short time; Inverse-compton photons are produced in the collision between these relativistic electrons and the ambient photons which have been emitted from the stellar p...
            对宇宙γ射线爆提出了如下的模型:宇宙γ射线爆发类似于太阳耀斑过程,但猛烈程度大得多;爆发时贮存在“耀斑”内的磁能转化为电子的动能;大量的高能电子在一个很短的时间内从“耀斑”飞出;这些高能电子在通过恒星周围的光子气体时,与光子气体相互碰撞,产生逆康普顿光子,形成γ射线爆。根据这一模型推导了γ射线爆的时间轮廓、能谱等的表达式,并对1972年4月27日事件作了应用。计算结果表明:在磁白矮星和O、B型热星上都可能出现γ射线爆。
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