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太阳表面米粒结构观测对比度分析 被引量:5
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作者 饶长辉 姜文汉 +1 位作者 凌宁 JacquesM.Beckers 《天文学报》 CSCD 北大核心 2001年第2期134-139,共6页
分析了观测系统焦面上和探测器所探测到的太阳表面米粒结构的对比度与观测系统口径、大气湍流相干长度以及系统探测灵敏度的关系 ,给出了不同口径、不同大气湍流相干长度以及不同系统探测灵敏度时的米粒结构对比度数值计算结果 .
关键词 太阳表面米粒结构 对比度 大气相干长度 光学传递函 大气湍流 太阳磁场活动
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太阳黑子千年一遇大爆发
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《物理通报》 2003年第11期23-23,共1页
关键词 太阳黑子 太阳磁场活动 太阳早期活动 宇宙射线 同位素 地球气候 全球变暖
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去看一场太阳系最绚烂的焰火
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作者 三叠纪小贝壳 《小学生时代》 2018年第2期24-27,共4页
新春佳节快到了,同学们都期待着看最美丽的焰火表演吧?哇,一束束火树银花在夜空中绚烂绽放,那转瞬即逝的缤纷色彩和炫酷造型,相信谁都会留下最美好的记忆。可是你知道吗,在我们地球妈妈生活的太阳系,有一种几乎每天都会爆发的漂亮焰火... 新春佳节快到了,同学们都期待着看最美丽的焰火表演吧?哇,一束束火树银花在夜空中绚烂绽放,那转瞬即逝的缤纷色彩和炫酷造型,相信谁都会留下最美好的记忆。可是你知道吗,在我们地球妈妈生活的太阳系,有一种几乎每天都会爆发的漂亮焰火,它无比巨大,比同学们看过的所有焰火都漂亮!而且每隔11年,这种太空焰火还会超级大爆发,地球上所有的烟花加在一起都没有它绚烂夺目!哈哈,别费心找啦,它就是我们头顶上太阳公公的杰作——太阳耀斑。 展开更多
关键词 焰火 太阳 太阳耀斑 绚烂夺目 一束束 头顶 太阳磁场 卡林顿 恒星活动 热等离子体
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Origin and structures of solar eruptions Ⅱ: Magnetic modeling 被引量:10
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作者 GUO Yang CHENG Xin DING MingDe 《Science China Earth Sciences》 SCIE EI CAS CSCD 2017年第8期1408-1439,共32页
The topology and dynamics of the three-dimensional magnetic field in the solar atmosphere govern various solar eruptive phenomena and activities, such as flares, coronal mass ejections, and filaments/prominences. We h... The topology and dynamics of the three-dimensional magnetic field in the solar atmosphere govern various solar eruptive phenomena and activities, such as flares, coronal mass ejections, and filaments/prominences. We have to observe and model the vector magnetic field to understand the structures and physical mechanisms of these solar activities. Vector magnetic fields on the photosphere are routinely observed via the polarized light, and inferred with the inversion of Stokes profiles. To analyze these vector magnetic fields, we need first to remove the 180° ambiguity of the transverse components and correct the projection effect. Then, the vector magnetic field can be served as the boundary conditions for a force-free field modeling after a proper preprocessing. The photospheric velocity field can also be derived from a time sequence of vector magnetic fields.Three-dimensional magnetic field could be derived and studied with theoretical force-free field models, numerical nonlinear force-free field models, magnetohydrostatic models, and magnetohydrodynamic models. Magnetic energy can be computed with three-dimensional magnetic field models or a time series of vector magnetic field. The magnetic topology is analyzed by pinpointing the positions of magnetic null points, bald patches, and quasi-separatrix layers. As a well conserved physical quantity,magnetic helicity can be computed with various methods, such as the finite volume method, discrete flux tube method, and helicity flux integration method. This quantity serves as a promising parameter characterizing the activity level of solar active regions. 展开更多
关键词 Solar activity Solar corona Coronal Mass Ejections(CMEs) Solar flares Magnetic fields Solar photosphere
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Predicting the solar maximum with the rising rate 被引量:3
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作者 DU ZhanLe WANG HuaNing 《Science China(Physics,Mechanics & Astronomy)》 SCIE EI CAS 2012年第2期365-370,共6页
The growth rate of solar activity in the early phase of a solar cycle has been known to be well correlated with the subsequent amplitude (solar maximum). It provides very useful information for a new solar cycle as ... The growth rate of solar activity in the early phase of a solar cycle has been known to be well correlated with the subsequent amplitude (solar maximum). It provides very useful information for a new solar cycle as its variation reflects the temporal evolution of the dynamic process of solar magnetic activities from the initial phase to the peak phase of the cycle. The correlation coefficient between the solar maximum (Rmax) and the rising rate (βa) at Am months after the solar minimum (Rmin) is studied and shown to increase as the cycle progresses with an inflection point (r = 0.83) at about Am = 20 months. The prediction error of Rmax based on βa is found within estimation at the 90% level of confidence and the relative prediction error will be less than 20% when Am ≥ 20. From the above relationship, the current cycle (24) is preliminarily predicted to peak around October, 2013 with a size of Rmax = 84 + 33 at the 90% level of confidence. 展开更多
关键词 solar physics solar activity sun spots solar cycles
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Analysis of the ionospheric variability based on wavelet decomposition 被引量:1
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作者 SHI Hao ZHANG DongHe +1 位作者 LIU YuMei HAO YongQiang 《Science China(Technological Sciences)》 SCIE EI CAS CSCD 2015年第1期174-180,共7页
In this work,the ionospheric variability is analyzed by applying the wavelet decomposition technique to the noontime fo F2,F10.7,interplanetary magnetic field(IMF)Bz,Ap,and lower thermospheric temperature at pressure ... In this work,the ionospheric variability is analyzed by applying the wavelet decomposition technique to the noontime fo F2,F10.7,interplanetary magnetic field(IMF)Bz,Ap,and lower thermospheric temperature at pressure of 10?4 h Pa in 2002.Results show that the variance of periodic oscillations in the ionosphere is largest in the 2–4-day period and declines with the increase of the period.The maximum variance of the periodic oscillations in solar irradiation is in the 16–32-day period.For geomagnetic activities,most of the variance is about equally distributed on intervals of periods shorter than 32 days.Variance distributions of IMF Bz and lower thermospheric temperature are similar to those of the ionosphere.They show the maximum in the 2–4-day period and decline with the increase of the period.By analyzing the distributions of the variances,the potential connections between the ionosphere and the external sources are discussed. 展开更多
关键词 IONOSPHERE VARIABILITY fo F2 Wavelet decomposition 2–32-day period
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