Authors: Ying Wang (NJIT), Yan Xu (NJIT), Ju Jing (NJIT), Haimin Wang(NJIT)

Polar crown filaments (PCFs) are crucially related to the structure of solar polar magnetic fields. They are physically significant because of the “rush-to-the-pole” motion, which is an indicator of the poleward drift of magnetic fields from decayed active regions. The formation and evolution of PCFs offer important insights into the Sun’s magnetic activity at high latitudes and the solar cycle variation. In this study, we present a statistical analysis of 42 PCFs eruptions. Our results show that: 1. Most PCFs (98%) disappeared via eruption, instead of thermal disappearance; 2. The majority of PCF eruptions were associated with slow CMEs (<800 km /s}); 3. Obvious rotation during the eruptions were noticed and the rotation directions agree with the numerical modeling. This is the evidence that flux ropes are formed; 4. For the eruptions with transient coronal holes, the estimated flux removed by the eruption is in the order of 10^20 to 10^21 Mx; 5. Time–distance analysis shows that 19 events exhibit a clear slow-rise to fast-rise transition, with typical onset heights of several tens to about 160 Mm and a mean onset velocity of about 3.5 km /s).