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Observations Supporting the Role of Magnetoconvection in Energy Supply to the Quiescent Solar Atmosphere View all abstracts by submitter

Scott McIntosh   Submitted: 2006-07-17 11:42

Identifying the two physical mechanisms behind the production and sustenance of the quiescent solar corona and solar wind poses two of the outstanding problems in solar physics today. We present analysis of spectroscopic observations from the Solar and Heliospheric Observatory (SOHO) that are consistent with a single physical mechanism being responsible for a significant portion of the heat supplied to the lower solar corona and the initial acceleration of the solar wind; the ubiquitous action of magnetoconvection-driven reprocessing and reconnection of the Sun's magnetic field. We deduce that the reconnection released plasma can either provide thermal input to the quiet solar corona or become a tributary to the solar wind is simply related to the global magnetic environment in which it is rooted.

Authors: Scott W. McIntosh, Alisdair R. Davey and Donald M. Hassler

Publication Status: Submitted
Last Modified: 2006-07-17 11:43
Go to main E-Print page  Statistical Study of the Reconnection Rate in Solar Flares Observed with YOHKOH/SXT  Simple Magnetic Flux Balance as an Indicator of Neon VIII Doppler Velocity Partitioning in an Equatorial Coronal Hole  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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