Meet my research

The twists of coronal mass ejection (CME)'s magnetic field lines are majorly injected during the magnetic reconnection in the low corona at the CME sources.

CME speed and kinetic energy are controlled by flare reconnection magnetic flux at their solar sources.  The flux from flare reconnection makes up 30% of the flux from the solar active region on average.

The solar cycle modulates CME erosion in the interplanetary medium. Heliospheric open flux may reconnect with CME flux ropes and cause its erosion.

CME’s magnetic properties are transported to CME flux ropes during magnetic reconnection at their sources. A one-to-one correspondence was found between CME field line rotation direction at their source and at Earth. 

We develop a CME forecasting model magnetic cloud prediction (MCP) model to predict the Earth-arrival time, propagation speed, and magnetic vectors of CMEs at Earth

Magnetic reconnection at CME sources may result in a highly twisted CME flux rope envelope. CME erosion may entirely peel away this envelope.

We study the initiation and erosion of a special kind of CME named Streamer blowout CME. We observe a multi-stage sympathetic breakout scenario. 

We investigate a complex-structured heliosphere and a nearly 'V'-shaped CME axis caused by deflection due to the presence of a coronal hole.