耀斑

基本解释 (translations)

flare

与耀斑相关的网络例句 [注：此内容来源于网络，仅供参考]

The applications of the theory in robot translation parameter computation and in Qualitative Scene Model construction are presented.(3) Intrinsic Images and color constancy of Real Color Images Based on the Dichromatic Reflection Model proposed by Klinker [55] , it is the NO. 1 for this paper to measure the spectral relationship of a CCD color camera, to reestablish the linear relationship, to separate the illuminant and object color components in real color images, and to extract the intrinsic image and highlight image from the real color image, as well as to eliminate the influences of highlights upon the usual image segmentation algorithm.

以Klinker[55]等提出的"双色反射模型"为基础，首次测定了彩色摄像机的光强----灰度响应关系，恢复了摄像机的整体线性关系；首次在真实彩色图像（即由彩色摄像机直接获取的图像）中成功地分离了光照和景物的颜色；成功地抽取了本色图像和耀斑图像；在此基础上，又将双色反射模型成功地运用到真实彩色图像的分割方面，消除了耀斑对分割的影响。

The HeⅠ 10830 profiles of the flare are relatively broad and can not be simulated by Doppler broadening mechanism with a uniform flare model atmosphere.

该耀斑的HeⅠ 10830谱线线翼相对较宽，不能用均匀耀斑模型的纯Doppler加宽机制解释。

Some people introduce subphotosphere magnetic charges or dipole, which can fit magnetic field on the photosphere, then the separatrix and separator above and on the photosphere can be located, the comparison between their location and location of flare ribbon support the idea of magnetic reconnection. It is called Source Method. Some people extrapolate magnetic fields of photosphere to corona by some method, then use QSLs method to investigate the relations between flare ribbons and magnetic field topology. Some people study relations between flare ribbons and singular point on the plane above photosphere. Some people investigate magnetic topology by analyzing magnetic field of photosphere directly.

或者以观测的光球磁场为基础，来构造光球下的磁荷或磁偶极等光球下磁源，进而研究光球上的磁拓扑结构与耀斑的关系；或者利用各种外推方法将光球磁场进行外推，然后用准分隔层的方法来研究磁拓扑结构与耀斑的关系；或者利用势场模型外推光球磁场，然后研究光球之上平行于光球的某一平面的两维奇点与耀斑的关系；或者直接利用观测的光球矢量场来研究磁场拓扑。

The total radiative loss include the sum of every possible transition between two levels under the atomical models of hydrogen (4 level + 1 continuum), ionized calcium (5 level + 1 continuum), and magnesium (3 level) beside the contributions from nagtive hydrogen of f-f and f-b tranditions.

并将辐射损失速率与非热电子束轰击和软x线作用下的产能率作了比较，结果表明：耀斑不同时刻的色球辐射损失变化可达一个量级以上；耀斑脉冲相前后电子束加热相当有效；耀斑强度极大时，电子束轰击和软x线加热都有作用；耀斑主相时，软x线加热更能有效地平衡辐射损失。

Five papers are included in the part, which entitled as semiempirical models of the impulsive phase of the chromospheric flare, a study of the energy deposits in flaring atmosphere with semiempirical models of flares, spectral line asymmetry of solar flare, combined study between SMM HXRBS observation and semiempirical models, and continuum emission of white-light flare.

论文的上篇由5篇文章组成，形成了研究耀斑半经验模型的一个系列，其内容除了构造半经验模型外，着重在半经验模型基础上作扩展性研究，包括探讨耀斑的能量过程，计算谱线轮廓的不对称性，讨论白光耀斑连续发射的大气特征，以及寻求高能观测结果与半经验模型的联系等。

The detailed time-match semiempirical models represnting the chromospheric state during the impulsive phase of the 2B flare on Fab. 3 1983 are proposed by making the non-LTE calculstions on hydrogen and ionized calcium. The physical pictures of total evolutionary pattern of the impulsivs phase of the flare are improved either quantitatively or qualitatively in comparison with the former work we did.

利用南京大学太阳塔多波段光谱仪拍摄到的1983年2月3日2B级耀斑脉冲相期间的Hα和CaⅡK线轮廓系列光谱资料，按照我们所发展的构造定态色球耀斑半经验模型的方法，通过联立求解氢和一次电离钙的能级平衡方程和辐射转移方程，建立了能够再生Hα和CaⅡK线观测轮廓的更为完整的1983年2月3日2B级耀斑脉冲相色球半经验模型。

The main characteristics include: the quiet Sun corona has a rapid response to the flare heating, within 2 second the corona temperature increases nearly one order of magnitude, but later such increase becomes very slowly; the downward velocity at early stage of impulsive phase is too small to be negnected; chromospheric evaporation made by conduction shows some intensely, the maximum evaporated velocity may be as large as 1000 km/s; the chromospheric condensation appears just when the chromospheric evaporation takes place and its place always coincide with that of transition region in the early stage; the maximum of chromospheric condensation occurs also in the early stage of impulsive phase, at which the density in condensation may be larger two order of magnitude than that of surround and the downward velocity may be as large as 100 km/s; after the maximum of chromospheric condensation, its strongth decreases gradually but its width becomes greater with time and have a tendency to transport into deep chromosphere; the front of chromospheric condensation heats atmosphere obviously and the temperature in the chromospheric condensation is higher than the original case; the downware velocity of transition region may be greater than 100 km/s at the early stage; when the evaporated material collide at the top of loop, the densityand the presure there increase rapidly, which result in the formation of a shock wave; and so on.

在改善色球辐射损失和精确分辨过渡区的基础上，通过联立求解连续性方程、动量方程和能量方程，构造了一维磁限制性耀斑环在热沉积作用下的大气动力学模型，获得了耀斑热模型下脉冲相早期较为细致的大气演化理论图象，其主要特征是：耀斑对宁静日冕的加热相当迅速，仅2秒钟日冕温度增加即达一个量级，之后日冕温度增加缓慢；脉冲相早期日冕向下速度很小，几乎可以忽略，热传导驱动色球蒸发，其过程较为激烈，蒸发极大速度可达到1000km/s；色球压缩区与色球蒸发几乎同时形成，且在早期其位置总是与过渡区位置重合；色球压缩极大发生在脉冲相早期，其时密度可高于周围约2个量级，向下速度可超过100km/s；色球压缩极大后，其强度逐渐减弱，但宽度明显增大，且渐渐脱离过渡区往色球传播；压缩区内物质温度要高于原先的大气温度；过渡区下降在脉冲相早期相当迅速，可超过100km/s；当蒸发物质在环顶高速相碰时，环顶的密度、压力迅速增大，且温度也有所增加，导致形成激波，其波面以每秒上百公里的速度自环顶向下传播；在脉冲相前期，日冕软x辐射对色球的加热作用可以忽略；等。

The second part pays attentions to the hydrodynamical model of solar flare (chromosphere+corona).

论文的下篇则致力于建立耀斑大气动力学理论模型，包括现有耀斑动力学模型评述，构造动力学模型的理论框架，耀斑主相动力学模型，以及耀斑脉冲相动力学模型等四章。

In the frame of constructing hydrodynamical model, some basic assumptions and equations were described in detail. Besides, there are three distinguish improvements above the former work: a new formula of chromosphere radiative loss was deduced out, which can roughly reproduce the results calculated by detailed non-LTE theory; a new physical process, i.e.

在构造耀斑动力学模型理论框架中，我们详细交待了基本假设和基本方程组，以及方程中各项的选取情况；针对现有耀斑动力学模型色球研究的不足，文中导得了新的色球辐射损失经验公式，它基本能够再生现有详细非局部热动平衡计算结果，较以前的处理方法有很大程度上的改善；引入了以前在耀斑环研究中从未被考虑过的日冕软x辐射加热色球的能量过程，推得了日冕软x辐射色球沉积的自恰公式。

Through the study on solar flare atmosphere, we may not only understand the energy process and various radiation properties, but also diagnostic the initial energy release and combine the study with the origin of solar flare.

通过对耀斑大气模型的研究，我们不〓可以搞清耀斑的能量过程和各种辐射性质，而且也可以探讨不同初始触发机制的后果，以与耀斑的起源联系起来。

与耀斑相关的网络解释 [注：此内容来源于网络，仅供参考]

flare：耀斑

太阳表面上耀斑(flare)也能廓. 例如奥米加星云(Omega Nebula),在人马座内(Sagittarius)发射强源"(focus)在地面下不过数公里深. 通常试验地下核爆炸,或探测海底油段时间叫做"隐生宙"(Cryptozoic Eon).

flares：耀斑

另一方面,Lockwood教授担忧的是,太阳活动相对平静时,其内部抑制的张力可能突然释放,即会突然产生猛烈的太阳爆发现象,如耀斑(flares)和日冕物质抛射(CME).

Solar flares：太阳耀斑

加州柏克莱大学Themis卫星组专案科学家马里特.奥列罗塞特(Marit Oieroset)表示:"裂缝的扩大速度非常快. "但有些类似的裂缝只是暂时的,2007年发现这个裂缝只裂开大约一个小时而已. 而太阳耀斑(Solar flares)对在轨道活动的太空员可能会构成潜在威胁,通常不会威胁到地面上人类的安全.

sun glint：太阳反辉区(卫星云图上的),太阳耀斑区(卫星云图上的)

sun elevation太阳仰角,太阳高度 | sun glint太阳反辉区(卫星云图上的),太阳耀斑区(卫星云图上的) | sun rise日出

Changed the menu option "flare explosions" to "flare effects：改变了菜单选项"耀斑爆炸"到"光晕效应

- Changed Hurry Up ships speeds a bit at high... | - Changed the menu option "flare explosions" to "flare effects" - 改变了菜单选项"耀斑爆炸"到"光晕效应" | - Changed Almost all the alien and big boss g...

plage flare：谱斑区耀斑

plage area 谱斑面积 | plage flare 谱斑区耀斑 | plagiarism 剽窃=>盗作, Using someone else''s work without giving proper credit.

white light flare：白光耀斑

white light event ==> 白光事件 | white light flare ==> 白光耀斑 | white light fluorescent lamp tube ==> 白光荧光灯管

Princeton Tec Sport Flare Dive Light (Blue)：普林斯顿tec体育耀斑潜水轻(蓝色)

Features: 特点: | Princeton Tec Sport Flare Dive Light (Blue)普林斯顿tec体育耀斑潜水轻(蓝色) | Top Quality - Manufactured to the highest specifications顶端质量-制造的最高规格

solar flare：太阳耀斑

太 阳耀斑(Solar flare)是一种最剧烈的太阳活动. 太阳表面突然出现亮斑闪耀,其寿命仅在几分钟到几十分钟之间,亮度上升迅速,减弱较慢. 一旦出现太阳耀斑,对於太阳 表面来说就是一次惊天动地的大爆发. 耀斑释放的能量相当於10万至100万次强火山爆发的总能量,

solar flare event：太阳耀斑效应

solar energy 太阳能 | solar flare event 太阳耀斑效应 | solar flare 太阳耀斑