TY  - GEN
A1  - Cheng, Xin
A1  - Zhang, Jie
A1  - Kliem, Bernhard
A1  - Török, Tibor
A1  - Xing, Chen
A1  - Zhou, Zhenjun
A1  - Inhester, Bernd
A1  - Ding, Mingde
T1  - Initiation and early kinematic evolution of solar eruptions
T2  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe
N2  - We investigate the initiation and early evolution of 12 solar eruptions, including six active-region hot channel and six quiescent filament eruptions, which were well observed by the Solar Dynamics Observatory, as well as by the Solar Terrestrial Relations Observatory for the latter. The sample includes one failed eruption and 11 coronal mass ejections, with velocities ranging from 493 to 2140 km s(-1). A detailed analysis of the eruption kinematics yields the following main results. (1) The early evolution of all events consists of a slow-rise phase followed by a main-acceleration phase, the height-time profiles of which differ markedly and can be best fit, respectively, by a linear and an exponential function. This indicates that different physical processes dominate in these phases, which is at variance with models that involve a single process. (2) The kinematic evolution of the eruptions tends to be synchronized with the flare light curve in both phases. The synchronization is often but not always close. A delayed onset of the impulsive flare phase is found in the majority of the filament eruptions (five out of six). This delay and its trend to be larger for slower eruptions favor ideal MHD instability models. (3) The average decay index at the onset heights of the main acceleration is close to the threshold of the torus instability for both groups of events (although, it is based on a tentative coronal field model for the hot channels), suggesting that this instability initiates and possibly drives the main acceleration.
T3  - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 1420 
KW  - solar coronal mass ejections
KW  - stellar coronal mass ejections
KW  - solar storm
Y1  - 2020
U6  - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-519720
SN  - 1866-8372
IS  - 2
ER  - 
TY  - JOUR
A1  - Cheng, Xin
A1  - Zhang, Jie
A1  - Kliem, Bernhard
A1  - Török, Tibor
A1  - Xing, Chen
A1  - Zhou, Zhenjun
A1  - Inhester, Bernd
A1  - Ding, Mingde
T1  - Initiation and early kinematic evolution of solar eruptions
JF  - The Astrophysical Journal
N2  - We investigate the initiation and early evolution of 12 solar eruptions, including six active-region hot channel and six quiescent filament eruptions, which were well observed by the Solar Dynamics Observatory, as well as by the Solar Terrestrial Relations Observatory for the latter. The sample includes one failed eruption and 11 coronal mass ejections, with velocities ranging from 493 to 2140 km s(-1). A detailed analysis of the eruption kinematics yields the following main results. (1) The early evolution of all events consists of a slow-rise phase followed by a main-acceleration phase, the height-time profiles of which differ markedly and can be best fit, respectively, by a linear and an exponential function. This indicates that different physical processes dominate in these phases, which is at variance with models that involve a single process. (2) The kinematic evolution of the eruptions tends to be synchronized with the flare light curve in both phases. The synchronization is often but not always close. A delayed onset of the impulsive flare phase is found in the majority of the filament eruptions (five out of six). This delay and its trend to be larger for slower eruptions favor ideal MHD instability models. (3) The average decay index at the onset heights of the main acceleration is close to the threshold of the torus instability for both groups of events (although, it is based on a tentative coronal field model for the hot channels), suggesting that this instability initiates and possibly drives the main acceleration.
KW  - solar coronal mass ejections
KW  - stellar coronal mass ejections
KW  - solar storm
Y1  - 2020
U6  - https://doi.org/10.3847/1538-4357/ab886a
SN  - 1055-6796
SN  - 1476-3540
VL  - 894
IS  - 2
SP  - 1
EP  - 20
PB  - Cambridge Scientific Publishers
CY  - Cambridge
ER  -