Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...334.1112j&link_type=abstract
Astronomy and Astrophysics, v.334, p.1112-1122 (1998)
Astronomy and Astrophysics
Astrophysics
50
Sun: Corona, Sun: Flares, Sun: X-Rays, Gamma Rays
Scientific paper
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.
Falewicz Robert
Fludra Andrzej
Jakimiec Jerzy
Phillips Kenneth J. H.
Tomczak Matthias
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