12 citations · 12 across the 6 of their papers we have counts for
7 papers
Magnetic Reconnection Governs the Entire Lifecycle of Solar Eruptive Magnetic Flux Rope
Xinkai Bian, Chaowei Jiang, Qingjun Liu +3
While magnetic flux ropes (MFRs) are widely accepted to exist prior to many solar eruptions, the physical mechanism responsible for triggering and subsequently driving their erupti…
An investigation of magnetic energy and helicity thresholds at the onset of solar eruptions based on numerical simulations
Xinkai Bian, Chaowei Jiang, Qingjun Liu +5
Identifying universal, topology-independent thresholds in the coronal magnetic fields at onset of solar eruptions is crucial for physics-based prediction of eruptions. To this end,…
MHD simulations of the slow-rise phase of solar eruptions initiated from a sheared magnetic arcade
Qingjun Liu, Chaowei Jiang, Zhipeng Liu
Before solar eruptions, a short-term slow-rise phase is often observed, during which the pre-eruption structure ascends at speeds much greater than the photospheric motions but muc…
A New Approach of Data-driven Simulation and Its Application to Solar Active Region 12673
Zhi-Peng Liu, Chao-Wei Jiang, Xin-Kai Bian +3
The solar coronal magnetic field is a pivotal element in the study of eruptive phenomena, and understanding its dynamic evolution has long been a focal point in solar physics. Nume…
Why are non-radial solar eruptions less frequent than radial ones?
Qingjun Liu, Chaowei Jiang, Xuesheng Feng +2
Coronal mass ejections from the Sun are not always initiated along a radial trajectory; such non-radial eruptions are well known to be caused by the asymmetry of the pre-eruption m…
A Model of Solar Magnetic Flux Rope Eruption Initiated Primarily by Magnetic Reconnection
Qingjun Liu, Chaowei Jiang, Xinkai Bian +3
There is a heated debate regarding the specific roles played by ideal magnetohydrodynamic (MHD) instability and magnetic reconnection in the causes of solar eruptions. In the conte…
Formation of Quiescent Prominence Magnetic Field by Supergranulations
Qingjun Liu, Chun Xia
To understand the formation of quiescent solar prominences, the origin of their magnetic field structures, i.e., magnetic flux ropes (MFRs), must be revealed. We use three-dimensio…