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Among the very bright transient events, solar X-ray
flares are the most relevant, comparable with the brightest GRBs.
An example of typical solar flare light curve is shown in fig. .
They distinguish from GRBs by their direction, of course, by
their long duration (typically ranging from s to some minutes)
and by their spectrum, which is softer than GRBs': this feature
in particular has turned out very effective to the aim of an
automatic identification (see next sections).
Example of solar X-ray flare detected by the GRBM, units 2+3,
on April 15, 2001, at 13:44 UT (upper panel: GRBM band; lower panel:
AC band). This flare shows a ``curious''
profile: the fast drop has been caused by the occultation of the Sun
behind the Earth, as seen from the BeppoSAX point of view.