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Numerical simulations of spicule formation in the solar atmosphere View all abstracts by submitter

Kris Murawski   Submitted: 2010-05-01 10:10

Context. We study the upward propagation of a localized velocity pulse that is initially launched below the transition region within the solar atmosphere. The pulse quickly steepens into a shock, which may lead to the formation of spicules. Aims. We aim to explore the spicule formation scenario in the framework of rebound shock model. Methods. We solve two-dimensional time-dependent magnetohydrodynamic equations numerically to find out spatial and temporal dynamics of spicules. Results. The numerical simulations show that the strong initial pulse may lead to the quasi periodic raising of chromospheric material into the lower corona in the form of spicules. The periodicity results from the nonlinear wake that is formed behind the pulse in the stratified atmosphere. The superposition of raising and falling off plasma portions resembles the time sequence of single and double (sometimes even triple) spicules, which is consistent with observational findings. Conclusions. The two-dimensional rebound shock model may explain the observed speed, width and heights of type I spicules as well as observed multi-structure and bi-directional flows. The model also predicts the appearance of spicules with 3 - 5 min period due to the consecutive shocks.

Authors: K. Murawski, T.V. Zaqarashvili
Projects: None

Publication Status: submitted
Last Modified: 2010-05-02 13:50
Go to main E-Print page  Testing magnetofrictional extrapolation with the Titov-D?moulin model of solar active regions  GeV Particle Acceleration in Solar Flares and Ground Level Enhancement (GLE) Events  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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