Reconnection-Driven Alfven (RDA) Waves in the Solar Corona

Details Reconnection-Driven Alfven (RDA) Waves in the Solar Corona Reconnection-Driven Alfven (RDA) Waves in the Solar Corona

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh31a1990e&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH31A-1990

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection

Scientific paper

The mechanisms for heating the corona and accelerating the solar wind remain active areas of solar and heliospheric research. Currently, two relatively distinct paradigms confront these problems: a waves/turbulence paradigm, and a magnetic reconnection/dissipation paradigm. The fact that magnetic reconnection generates Alfvén waves suggests that the heating of the low-beta corona and the acceleration of the wind are likely the result of both paradigms operating simultaneously. This research aims to unify the two competing viewpoints. We present 3D MHD simulations of magnetic reconnection/dissipation processes in the solar corona that provide a self-consistent mechanism for producing the energy injection spectrum required by the waves/turbulence paradigm. We analyze the simulations to quantify the amount of magnetic energy released in the reconnection process and the material and energy fluxes carried by large-amplitude, nonlinear, reconnection-driven Alfvén (RDA) waves. In addition to isolating the RDA waves, characterizing their physical properties, and investigating their evolution in a low-beta, gravitationally stratified model corona, we examine their time-dependent material and energy outflows and discuss their observable consequences in the corona and inner heliosphere.

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