论文标题
图像仪在Parker太阳能探针和太阳陆地关系天文台上观察到的流板驱散CME的演变
Evolution of a Streamer-Blowout CME as Observed by Imagers on Parker Solar Probe and the Solar Terrestrial Relations Observatory
论文作者
论文摘要
上下文：2020年1月26日至27日，宽阔的图像仪WISPR关于Parker太阳能探测器（PSP）观察到冠状质量弹射（CME），距离大约30个太阳能半径的距离，当时它通过了该乐器的95度视野视野，提供了前所未有的磁带式磁带的视图。从1月25日开始，立体声也看到了同一CME。 目的：我们的目标是了解起源并确定此CME的轨迹。 方法：我们分析了三个位置良好的航天器的数据：帕克太阳能探针（PSP），太阳陆地关系天文台 - 磁头（Stereo-A）和太阳能动力学天文台（SDO）。使用Liewer等人中描述的方法确定CME轨迹。 （2020）并使用立体声A的CME传播的同时图像进行了验证。与立体声A的偶然对齐还提供了导致喷发的冠状活动的看法。从1月25日，使用CORONA的潜在磁场模型，SDO的观察结果与电晕的潜在磁场模型一起分析了冠状磁性演化的三天。 结果：我们发现1月25日CME可能是1月23日开始的缓慢磁通绳爆发的最终结果，并通过Stereo-A/Extreme Ultraviolet Imager（EUVI）观察到。对这些观察结果的分析表明，在1月25日最终弹出之前的一天以上，磁通绳显然受到了限制。在1月25日爆发之前几个小时，立体声A/COR2观察到上覆的彩带的肿胀和增亮，这使我们将其归类为流媒体驱动的CME。对SDO数据的分析表明，由新兴的活性区域引起的冠状磁场的重组导致通量绳的最终弹出。
Context: On 26-27 January 2020, the wide-field imager WISPR on Parker Solar Probe (PSP) observed a coronal mass ejection (CME) from a distance of approximately 30 solar radii as it passed through the instrument's 95 degree field-of-view, providing an unprecedented view of the flux rope morphology of the CME's internal structure. The same CME was seen by STEREO, beginning on 25 January. Aims: Our goal was to understand the origin and determine the trajectory of this CME. Methods: We analyzed data from three well-placed spacecraft: Parker Solar Probe (PSP), Solar Terrestrial Relations Observatory-Ahead (STEREO-A), and Solar Dynamics Observatory (SDO). The CME trajectory was determined using the method described in Liewer et al. (2020) and verified using simultaneous images of the CME propagation from STEREO-A. The fortuitous alignment with STEREO-A also provided views of coronal activity leading up to the eruption. Observations from SDO, in conjunction with potential magnetic field models of the corona, were used to analyze the coronal magnetic evolution for the three days leading up to the flux rope ejection from the corona on 25 January. Results: We found that the 25 January CME is likely the end result of a slow magnetic flux rope eruption that began on 23 January and was observed by STEREO-A/Extreme Ultraviolet Imager (EUVI). Analysis of these observations suggest that the flux rope was apparently constrained in the corona for more than a day before its final ejection on 25 January. STEREO-A/COR2 observations of swelling and brightening of the overlying streamer for several hours prior to eruption on January 25 led us to classify this as a streamer-blowout CME. The analysis of the SDO data suggests that restructuring of the coronal magnetic fields caused by an emerging active region led to the final ejection of the flux rope.
