  Coronal mass ejections (CMEs), which are among the most magnificent solar
eruptions, are a major driver of space weather and can thus affect diverse
human technologies. Different processes have been proposed to explain the
initiation and release of CMEs from solar active regions (ARs), without
reaching consensus on which is the predominant scenario, and thus rendering
impossible to accurately predict when a CME is going to erupt from a given AR.
To investigate AR magnetic properties that favor CMEs production, we employ
multi-spacecraft data to analyze a long duration AR (NOAA 11089, 11100, 11106,
11112 and 11121) throughout its complete lifetime, spanning five Carrington
rotations from July to November 2010. We use data from the Solar Dynamics
Observatory to study the evolution of the AR magnetic properties during the
five near-side passages, and a proxy to follow the magnetic flux changes when
no magnetograms are available, i.e. during far-side transits. We characterized
the angular widths, speeds and masses of 108 CMEs that we associated to the AR,
when examining a 124-day period. Such an ejectivity tracking was possible
thanks to the multiviewpoint images provided by the STEREO and SOHO in a
quasiquadrature configuration. We also inspected the X-ray flares registered by
the GOES satellite and found 162 to be associated to the AR under study. Given
the substantial number of ejections studied, we use a statistical approach
instead of a single-event analysis. We found three well defined periods of very
high CMEs activity and two periods with no mass ejections that are preceded or
accompanied by characteristic changes in the AR magnetic flux, free magnetic
energy and/or presence of electric currents. Our large sample of CMEs and long
term study of a single AR, provide further evidence relating AR magnetic
activity to CME and Flare production.
