Abstract
The solar corona is populated by a large number of semitoroidal magnetic loops, some of which are sufficiently close to each other within a neighborhood that the probability of loop-to-loop interaction is not negligible. The interaction of two coronal loops is studied using a three-dimensional numerical simulation. The first loop is an established, current-carrying magnetic loop in hydromagnetic equilibrium. The second loop dynamically emerges from the photosphere in the same neighborhood. There are a large number of possible configurations in a two-loop system regarding their relative orientation, physical size, and directions of their toroidal magnetic field and electric current. We present three representative, but characteristically different, configurations whose interactions result in releasing various amounts of energy stored in the magnetic field. Using typical coronal parameters, some of them can take place in a relatively short timescale and release sufficient energy to account for a small flare.
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