SXR CORONAL FLASHES

We provide evidence for the existence of a new type of soft X-ray (SXR ) brightening event that we call coronal flashes. The phenomenon was o bserved on deep time series taken with the SXT of Yohkoh in the north polar coronal hole, near the sunspot minimum. Events last as short as 1.5 mn and the corresponding SXR flux span the range of energies, from single pixel brightenings corresponding to fluxes of about 10(24) erg but barely surpassing the level of the noise, to higher and more smea red multiple pr brightenings still orders of magnitude smaller than th e known small SXR bright points and/or transient brightenings. The typ ical occurrence rate of flashes is 1 event/arcmin(2)/5mn with a 1/2 mn integration time. At least part of the coronal flashes are recurrent and some of them could be associated with a SXR jet; it is not clear w hat is their optical counterpart.