In addition to acting as an early warning for geomagnetic storms,
GBSRBS aims to further shed light on a variety of phenomena arising from
magnetic activity near the base of the Solar corona such as the
catastrophic release of energy that accompanies rapid magnetic
reconnection there, the flares resulting from beams of electrons
accelerated along the broken field lines, and the burst activity
caused by the magnetohydrodynamic shock waves accompanying the
flares. The precursors of CME and surface filament-formations may
also be studied. The close connection between emission frequency
and positioning of energy release afforded by the fact that such
events take place in a plasma allows GBSRBS to contribute to our
knowledge of the structure of the corona and its behavior under
the extreme conditions that arise during flare activity.
Above all, GBSRBS will aid in answering the questions of exactly where and how
energy is released in coronal burst events. It is hoped that, due
to the abundance and easy accessibility of such high-quality
broadband spectra, coupled with the increased opportunity for
data-pooling with other Solar observatories ( WIND, ACE, RHESSI,
SOHO, TRACE, Ulysses), researchers from around the world will be
able to take advantage of a more fully integrated view of the
processes that occur in the fascinating environment of our planet's star.
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