A time series of filament eruptions observed by three eyes from space:from failed to successful eruptions  

作　　者：Yuan-DengShen YuLiu RuiLiu 

机构地区：[1]NationalAstronomicalObservatories／YunnanObservatory,ChineseAcademyofSciences,Kunming650011,China [2]GraduateUniversityofChineseAcademyofSciences,Beijing100049,China [3]SpaceWeatherResearchLaboratory,NewJerseyInstituteofTechnology,UniversityHeights,Newark,NJ07102—1982,USA

出　　处：《Research in Astronomy and Astrophysics》2011年第5期594-606,共13页天文和天体物理学研究（英文版）

基　　金：supported by the Chinese foundations MOST (2011CB811400);the National Natural Science Foundation of China (Grant Nos. 10933003,11078004 and 11073050)

摘　　要：We present stereoscopic observations of six sequential eruptions of a filament in the active region NOAA 11045 on 2010 Feb 8, with the advantage of the STEREO twin viewpoints in combination with Earth＇s viewpoint from SOHO instruments and ground-based telescopes. The last one of the six eruptions is a coronal mass ejection, but the others are not. The flare in this successful one is more intense than in the others. Moreover, the velocity of filament material in the successful one is also the largest among them. Interestingly, all the filament velocities are found to be proportional to the power of their flares. We calculate magnetic field intensity at low altitude, the decay indexes of the external field above the filament, and the asymmetry properties of the overlying fields before and after the failed eruptions and find little difference between them, indicating the same coronal confinement exists for both the failed and successful eruptions. The results suggest that, besides the confinement of the coronal magnetic field, the energy released in the low corona should be another crucial element affecting a failed or successful filament eruption. That is, a coronal mass ejection can only be launched if the energy released exceeds some critical value, given the same initial coronal conditions.We present stereoscopic observations of six sequential eruptions of a filament in the active region NOAA 11045 on 2010 Feb 8, with the advantage of the STEREO twin viewpoints in combination with Earth＇s viewpoint from SOHO instruments and ground-based telescopes. The last one of the six eruptions is a coronal mass ejection, but the others are not. The flare in this successful one is more intense than in the others. Moreover, the velocity of filament material in the successful one is also the largest among them. Interestingly, all the filament velocities are found to be proportional to the power of their flares. We calculate magnetic field intensity at low altitude, the decay indexes of the external field above the filament, and the asymmetry properties of the overlying fields before and after the failed eruptions and find little difference between them, indicating the same coronal confinement exists for both the failed and successful eruptions. The results suggest that, besides the confinement of the coronal magnetic field, the energy released in the low corona should be another crucial element affecting a failed or successful filament eruption. That is, a coronal mass ejection can only be launched if the energy released exceeds some critical value, given the same initial coronal conditions.

关 键 词：Sun： filaments - Sun： corona- Sun： magnetic fields - Sun： flares -Sun： coronal mass ejections （CMEs） 

分 类 号：P145.3[天文地球—天体物理] O211.61[天文地球—天文学]