To better understand the dynamical process of active-region filament eruptions and associated flares and CMEs , we carried out a statistical study of 120 events observed by Big Bear Solar Observatory ( BBSO ) , Transition Region and Coronal Explorer ( TRACE ) , and the Extreme-ultraviolet Imaging Telescope ( EIT ) on board Solar and Heliospheric Observatory ( SOHO ) from 1998 to 2007 .
We combined filament observations with the NOAA ’ s flare reports , Michelson Doppler Imager ( MDI ) magnetograms , and Large Angle and Spectrometric Coronagraph ( LASCO ) data , to investigate the relationship between active-region filament eruptions and other solar activities .
We found that 115 out of 120 ( about 96 % ) filament eruptions are associated with flares .
56 out of 105 ( about 53 % ) filament eruptions are found to be associated with CMEs except for 15 events without corresponding LASCO data .
We note the limitation of coronagraphs duo to geometry or sensitivity , leading to many smaller CMEs that are Earth-directed or well out of the plane of sky not being detected by near-Earth spacecraft .
Excluding those without corresponding LASCO data , the CME association rate of active-region filament eruptions clearly increases with X-ray flare class from about 32 % for C-class flares to 100 % for X-class flares .
We also found that the eruptions of active-region filaments associated with Halo CMEs are often accompanied by large flares ( 18 out of 20 events ; \geq M1.0 ) .
About 92 % events ( 11 out of 12 ) associated with X-class flare are associated with Halo CMEs .
Such a result is due to that the Earth-directed CMEs detected as Halo CMEs are often the larger CMEs and many of the smaller ones are not detected because of the geometry and low intensity .
The average speed of the associated CMEs of filament eruptions increases with X-ray flare size from 563.7 km/s for C-class flares to 1506.6 km/s for X-class flares .
Excluding the active region located in the area more than 50 degrees from the solar center and 5 without corresponding MDI data , the \beta magnetic field configuration ( about 47 % ; 36 out of 77 ) is more likely to form eruptive filaments than other ones and there are 33 filament eruptions associated with magnetic flux cancellation , 42 events associated with magnetic flux emergence , 2 events without variation of magnetic field .
The average area of emergence regions is 855.9 square arcseconds .
These findings may be instructive to not only in respect to the modeling of active-region filament eruptions but also in predicting flares and CMEs .