Predicting the Onset of Solar Eruptions

Details Predicting the Onset of Solar Eruptions Predicting the Onset of Solar Eruptions

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1043..245f&link_type=abstract

EXPLORING THE SOLAR SYSTEM AND THE UNIVERSE. AIP Conference Proceedings, Volume 1043, pp. 245-251 (2008).

Other

Flares, Corona, Magnetohydrodynamics And Plasmas, Chromosphere, Astronomical Observations

Scientific paper

Large solar eruptions, including those that produce coronal mass ejections, are most likely the result of a rapid release of magnetic energy stored in the corona. A primary puzzle regarding such a process is the identity of the mechanism that triggers the energy release and initiates the eruption. One possibility is the onset of an ideal-MHD instability or, more generally, the loss of an ideal-MHD equilibrium. A mechanism of this type would easily account for the fact that large eruptions typically occur on the Alfvén timescale of the corona. Another possibility is the onset of a resistive instability that involves magnetic reconnection. Models of both types have recently been developed. Hybrid models that involve ideal and resistive processes acting in tandem are also plausible.

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