Twisted flux tube emergence from the convection zone to the corona II: Later states

Details Twisted flux tube emergence from the convection zone to the corona II: Later states Twisted flux tube emergence from the convection zone to the corona II: Later states

2009-06-30

arxiv.org/abs/0906.5464v1

Astrophys.J.702:129-140,2009

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

31 pages, 12 figures, accepted in ApJ

Scientific paper

10.1088/0004-637X/702/1/129

3D simulations of magnetic flux emergence are carried out in a computational domain spanning the upper layers of the convection zone to the lower corona. We use the Oslo Staggered Code to solve the full MHD equations with non-grey and NLTE radiative transfer and thermal conduction along the magnetic field lines. In this paper we concentrate on the later stages of the simulations and study the evolution of the structure of the rising flux in the upper chromosphere and corona, the interaction between the emerging flux and the weak coronal magnetic field initially present, and the associated dynamics. The flux tube injected at the bottom boundary rises to the photosphere where it largely remains. However, some parts of the flux tube become unstable and expand in patches into the upper chromosphere. The flux rapidly expands towards the corona, pushing the coronal and transition region material aside, lifting and maintaining the transition region at heights greater than 5 Mm above the photosphere for extensive periods of time. The pre-existing magnetic field in the corona and transition region is perturbed by the incoming flux and reoriented by a series of high Joule heating events. Low density structures form in the corona while at later times a high density filamentary structure appears in the lower part of the expanding flux. The dynamics of these and other structures is discussed. While Joule heating due to the expanding flux is episodic, it increases in relative strength as fresh magnetic field rises and becomes energetically important in the upper chromosphere and corona at later times. Chromospheric, transition region and coronal lines are computed and their response to the perturbation caused by the expanding emerging flux is discussed.

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