论文标题
使用修订后的锥体模型跟踪光环冠状质量射血的3D演变
Tracking the 3D evolution of a halo coronal mass ejection using the revised cone model
论文作者
论文摘要
This paper aims to track the 3D evolution of a full halo CME on 2011 June 21. The CME results from a non-radial eruption of a filament-carrying flux rope in NOAA active region 11236. The eruption is observed in EUV wavelengths by the EUVI on board the ahead and behind STEREO spacecrafts and the AIA on board SDO. CME由立体声板上的COR1冠冕和船上的C2 Coronagraph观察到SOHO/LASCO。修订后的锥体模型略微修饰，锥的顶部变成了一个球体，在内部与腿部切线。使用多点观测值，应用锥模型来得出CME的形态和运动学特性。圆锥形形状与Euvi和Cor1在板立体观察到的CME非常吻合，并在板立体声双航天器和Lasco/C2 Coronagraph上观察到。锥角度从初始阶段的54 $^{\ circ} $急剧增加到130 $^{\ circ} $，表明快速扩展。 CME领先前沿的锥角度和中心距离之间的关系，$ω= 130 \ degr-480d^{ - 5} $，其中$ d $属于$ r _ {\ odot} $的单位。倾斜角度从$ \ sim $ 51 $^{\ circ} $逐渐降低到$ \ sim $ 18 $^{\ circ} $，这表明了径向传播的趋势。 HeliPentric距离在初始阶段逐渐增加，并在后期阶段迅速增加到$ \ sim $ 11 \，$ r _ {\ odot} $。 CME的真实速度达到$ \ sim $ 1140 km s $^{ - 1} $，是$ \ sim $ 1.6 $ 1.6倍，比LASCO/C2视图中的明显速度高。修订后的模型有望在跟踪CME的完整演变方面。
This paper aims to track the 3D evolution of a full halo CME on 2011 June 21. The CME results from a non-radial eruption of a filament-carrying flux rope in NOAA active region 11236. The eruption is observed in EUV wavelengths by the EUVI on board the ahead and behind STEREO spacecrafts and the AIA on board SDO. The CME is observed by the COR1 coronagraph on board STEREO and the C2 coronagraph on board SOHO/LASCO. The revised cone model is slightly modified, with the top of the cone becoming a sphere, which is internally tangent to the legs. Using the multi-point observations, the cone model is applied to derive the morphological and kinematic properties of the CME. The cone shape fits nicely with the CME observed by EUVI and COR1 on board STEREO twin spacecraft and LASCO/C2 coronagraph. The cone angle increases sharply from 54$^{\circ}$ to 130$^{\circ}$ in the initial phase, indicating a rapid expansion. A relation between the cone angle and heliocentric distance of CME leading front is derived, $ω=130\degr-480d^{-5}$, where $d$ is in unit of $R_{\odot}$. The inclination angle decreases gradually from $\sim$51$^{\circ}$ to $\sim$18$^{\circ}$, suggesting a trend of radial propagation. The heliocentric distance increases gradually in the initial phase and quickly in the later phase up to $\sim$11\,$R_{\odot}$. The true speed of CME reaches $\sim$1140 km s$^{-1}$, which is $\sim$1.6 times higher than the apparent speed in the LASCO/C2 field of view. The revised model is promising in tracking the complete evolution of CMEs.
