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Title: MORPHOLOGY AND DYNAMICS OF SOLAR PROMINENCES FROM 3D MHD SIMULATIONS

In this paper we present a numerical study of the time evolution of solar prominences embedded in sheared magnetic arcades. The prominence is represented by a density enhancement in a background-stratified atmosphere and is connected to the photosphere through the magnetic field. By solving the ideal magnetohydrodynamic equations in three dimensions, we study the dynamics for a range of parameters representative of real prominences. Depending on the parameters considered, we find prominences that are suspended above the photosphere, i.e., detached prominences, but also configurations resembling curtain or hedgerow prominences whose material continuously connects to the photosphere. The plasma-β is an important parameter that determines the shape of the structure. In many cases magnetic Rayleigh-Taylor instabilities and oscillatory phenomena develop. Fingers and plumes are generated, affecting the whole prominence body and producing vertical structures in an essentially horizontal magnetic field. However, magnetic shear is able to reduce or even to suppress this instability.
Authors:
; ; ;  [1] ;  [2]
  1. Departament de Física, Universitat de les Illes Balears, E-07122 Palma de Mallorca (Spain)
  2. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife (Spain)
Publication Date:
OSTI Identifier:
22364454
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 799; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DENSITY; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; MORPHOLOGY; NUMERICAL ANALYSIS; PHOTOSPHERE; PLASMA; RAYLEIGH-TAYLOR INSTABILITY; SHEAR; SOLAR PROMINENCES; STAR EVOLUTION; SUN