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SOLAR PROMINENCE MERGING Guillaume Aulanier
 

Summary: SOLAR PROMINENCE MERGING
Guillaume Aulanier
Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris, 92195 Meudon Cedex, France;
guillaume.aulanier@obspm.fr
and
C. Richard DeVore1
and Spiro K. Antiochos2
Naval Research Laboratory, Washington DC 20375
Received 2006 January 27; accepted 2006 April 7
ABSTRACT
In a recent paper, we described MHD simulations of the interaction between a pair of distinct prominences
formed by the photospheric line-tied shearing of two separated dipoles. One case was typical of solar observations
of prominence merging, in which the prominences have the same axial field direction and sign of magnetic helicity.
For that configuration, we reported the formation of linkages between the prominences due to magnetic recon-
nection of their sheared fields. In this paper, we analyze the evolution of the plasma-supporting magnetic dips in this
configuration. As the photospheric flux is being progressively sheared, dip-related chromospheric fibrils and high-
altitude threads form and develop into the two prominences, which undergo internal oscillations. As the prom-
inences are stretched farther along their axes, they come into contact and their sheared fluxes pass each other, and
new dips form in the interaction region. The distribution of these dips increasingly fills the volume between the
prominences, so that the two progenitors gradually merge into a single prominence. Our model reproduces typical

  

Source: Aulanier, Guillaume - Observatoire de Paris

 

Collections: Physics