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Imaging solar coronal condensation forming prominences was difficult in thepast, a situation recently changed by Hinode and SDO. We present the firstexample observed with SDO/AIA, in which material gradually cools throughmultiple EUV channels in a transequatorial loop system that confines an earliereruption. Nine hours later, this leads to eventual condensation at the dip ofthese loops, forming a moderate-size prominence of ~$10^{14}$ gram, to becompared to the characteristic $10^{15}$ gram mass of a CME. The prominencemass is not static but maintained by condensation at a high estimated rate of$10^{10}$ gram/sec against a comparable, sustained drainage through numerousvertical downflow threads, such that 96% of the total condensation (~$10^{15}$gram) is drained in approximately one day. The mass condensation and drainagerates temporally correlate with the total prominence mass. The downflowvelocity has a narrow Gaussian distribution with a mean of 30 km/s, while thedownward acceleration distribution has an exponential drop with a mean of ~1/6$g_{Sun}$, indicating a significant canceling of gravity, possibly by theLorentz force. Our observations show that a macroscopic quiescent prominence ismicroscopically dynamic, involving the passage of a significant mass throughit, maintained by a continual mass supply against a comparable mass drainage,which bears important implications for CME initiation mechanisms in which massunloading is important.

First SDO/AIA Observation of Solar Prominence Formation Following an Eruption: Magnetic Dips and Sustained Condensation and Drainage