  In this paper, we identified the magnetic source locations of 142 quasi-
homologous (QH) coronal mass ejections (CMEs), of which 121 are from solar
cycle (SC) 23 and 21 from SC 24. Among those CMEs, 63% originated from the same
source location as their predecessor (defined as S-type), while 37% origi-
nated from a different location within the same active region as their
predecessor (defined as D-type). Their distinctly different waiting time
distribution, peaking around 7.5 and 1.5 hours for S- and D-type CMEs, suggests
that they might involve different physical mechanisms with different
characteristic time scales. Through detailed analysis based on non-linear force
free (NLFF) coronal mag- netic field modeling of two exemplary cases, we
propose that the S-type QH CMES might involve a recurring energy release
process from the same source location (by magnetic free energy replenishment),
whereas the D-type QH CMEs can happen when a flux tube system disturbed by a
nearby CME.

Solar and Stellar Astrophysics