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首页> 外文期刊>Solar physics >Variation in Coronal Activity from Solar Cycle 24 Minimum to Maximum Using Three-Dimensional Reconstructions of the Coronal Electron Density from STEREO/COR1
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Variation in Coronal Activity from Solar Cycle 24 Minimum to Maximum Using Three-Dimensional Reconstructions of the Coronal Electron Density from STEREO/COR1

机译:从STEREO / COR1的冠状电子密度的三维重建,太阳循环24的冠状活动变化最小到最大值

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摘要

Three-dimensional electron density distributions in the solar corona are reconstructed for 100 Carrington rotations (CR 2054-2153) during 2007/03 - 2014/08 using the spherically symmetric method from polarized white-light observations with the inner coronagraph (COR1) onboard the twin Solar Terrestrial Relations Observatory (STEREO). These three-dimensional electron density distributions are validated by comparison with similar density models derived using other methods such as tomography and a magnetohydrodynamics (MHD) model as well as using data from the Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO)-C2. Uncertainties in the estimated total mass of the global corona are analyzed based on differences between the density distributions for COR1-A and -B. Long-term variations of coronal activity in terms of the global and hemispheric average electron densities (equivalent to the total coronal mass) reveal a hemispheric asymmetry during the rising phase of Solar Cycle 24, with the northern hemisphere leading the southern hemisphere by a phase shift of 7 -9 months. Using 14 CR (approximate to 13-month) running averages, the amplitudes of the variation in average electron density between Cycle 24 maximum and Cycle 23/24 minimum (called the modulation factors) are found to be in the range of 1.6-4.3. These modulation factors are latitudinally dependent, being largest in polar regions and smallest in the equatorial region. These modulation factors also show a hemispheric asymmetry: they are somewhat larger in the southern hemisphere. The wavelet analysis shows that the short-term quasi-periodic oscillations during the rising and maximum phases of Cycle 24 have a dominant period of 7-8 months. In addition, it is found that the radial distribution of the mean electron density for streamers at Cycle 24 maximum is only slightly larger (by approximate to 30%) than at cycle minimum.
机译:在2007/03-2014 / 08期间,使用来自偏振的白光观测(Cor1)的球形对称方法在2007/03-2014 / 08期间重建太阳能电晕中的三维电子密度分布(CR 2054-2153)。双太阳陆地关系天文台(立体声)。通过使用其他方法(如断层摄影和磁流动动力学(MHD)模型(MHD)模型(SOHO)/大角度和光谱凝血件(SOHO)/磁性流体模型(MHD)/大角度和光谱凝血性( Lasco)-C2。基于COR1-A和-B的密度分布与-B的差异分析了全球电晕总质量的不确定性。在全局和半球平均电子密度(相当于总冠状质量)方面的长期变化揭示了太阳循环24的上升期间的半球不对称,北半球通过相移南半球7-9个月。使用14 Cr(近似为13个月)运行平均值,发现循环24之间的平均电子密度变化的幅度最大和循环23/24最小(称为调制因子)在1.6-4.3的范围内。这些调制因子是纬向的,在极地区域中最大,并且在赤道区域中最小。这些调节因子也显示出半球不对称:南半球在稍微较大。小波分析表明,在循环24的上升和最大阶段期间的短期准周期性振荡具有7-8个月的优势。另外,发现循环24在循环24最大值的平均电子密度的径向分布仅略大(近似为30%),而不是在最小循环。

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