The kink instability of a coronal magnetic loop as a trigger mechanism for solar eruptions

Details The kink instability of a coronal magnetic loop as a trigger mechanism for solar eruptions The kink instability of a coronal magnetic loop as a trigger mechanism for solar eruptions

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004padeu..14..165t&link_type=abstract

In: Proceedings of the British-Hungarian N+N Workshop for Young Researchers On Computer processing and use of satellite data in

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The kink instability of twisted magnetic flux tubes in the solar corona is regarded as a possible initiation process of solar eruptions. We study the stability properties and the dynamic evolution of such coronal magnetic loops using 3D numerical simulations within the framework of ideal MHD. The analytical force-free coronal loop model by Titov and Demoulin (1999) is used as initial condition in the simulations. The loop model is found to be kink-unstable if a critical twist is exceeded. The growing kink perturbation leads to the formation of current sheets, which steepen exponentially and define the locations of plasma heating. Due to the twist in the magnetic field, the heated structures are S shaped - in very good agreement with soft X-ray observations of solar eruptions. The model, however, does not yet show a successful eruption, rather the kink instability starts to saturate. We present an improvement of the model which is promising with regard to eruption: a modification of the equilibrium so that the magnetic field surrounding the loop decreases more rapidly with height above the photosphere. Furthermore, we briefly discuss how the simulation results can be related to observations of solar eruptive phenomena.

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