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THE BRIGHT LOOP-TOP KERNELS IN YOHKOH X-RAY FLARES

We have investigated loop-top kernels of the soft X– ray emission seen in the Yohkoh Soft X-ray Telescope (SXT) images. Detailed comparison of the observations from various Yohkoh instruments shows that these kernels contain two kinds of flare plasma: a cooler (∼ 10 MK) and a hotter (∼ 20 MK) one. The cooler plasma plays a dominant role in the emission recorded by the SXT and the hotter plasma is responsible for the Fe xxv emission and the emission recorded by Hard X–ray Telescope 14-23 keV band during the post-impulsive phase of a flare. We argue that the best model, which is in agreement with the above observational results, is a turbulent model of a flare loop-top kernel. The magnetic field is tangled in the kernel and a number of transient current sheets occur there. The hotter (∼ 20 MK) plasma is contained in the current sheets and they are surrounded by the cooler (∼ 10 MK) plasma. The turbulent model of the flare loop-top kernel also allows us to explain why the kernels are brighter than the “legs” connecting them with the chromosphere.