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Aims. We study the emergence of a non-twisted flux tube from the solarinterior into the solar atmosphere. We investigate whether the length of thebuoyant part of the flux tube (i.e. {\lambda}) affects the emergence of thefield and the dynamics of the evolving magnetic flux system. Methods. Weperform three-dimensional (3D), time-dependent, resistive, compressible MHDsimulations using the Lare3D code. Results. We find that there are considerabledifferences in the dynamics of the emergence of a magnetic flux tube when{\lambda} is varied. In the solar interior, for larger values of {\lambda}, therising magnetic field emerges faster and expands more due to its lower magnetictension. As a result, its field strength decreases and its emergence above thephotosphere occurs later than in the smaller {\lambda} case. However, in bothcases, the emerging field at the photosphere becomes unstable in two places,forming two magnetic bipoles that interact dynamically during the evolution ofthe system. Most of the dynamic phenomena occur at the current layer, which isformed at the interface between the interacting bipoles. We find the formationand ejection of plasmoids, the onset of successive jets from the interface, andthe impulsive heating of the plasma in the solar atmosphere. We discuss thetriggering mechanism of the jets and the atmospheric response to the emergenceof magnetic flux in the two cases.

Emergence of non-twisted magnetic fields in the Sun: Jets and atmospheric response