Observational Analysis of the Relation between Coronal Loop
Heating and Photospheric Magnetic Fields
Yukio Katsukawa
The solar corona and the photosphere are linked through magnetic field
lines, and heating energy is supposed to be supplied from the footpoints
of each coronal loop alog magnetic field lines. Thus it is important to
examine properties of photospheric magnetic fields at the footpoints of
the coronal loops in order to understand heating of the coronal loops. We
performed simultaneous observations of photospheric magnetic properties
and coronal loop structures with Advanced Stokes Polarimeter (ASP) and
TRACE. We found that (1) the difference between hot and cool coronal
loops was related with number density of elemental magnetic elements at
the loop footpoints in the photosphere (Katsukawa and Tsuneta 2005), and
(2) the cool coronal loops emanating from a sunspot had their footpoints
at the positions where there was highly interlaced magnetic structure
around an umbra (Katsuakwa et al. 2005). These observational results
suggest that critical magnetic properties are not yet spatially resolved
to understand the coronal heating. Solar-B will provide an opportunity to
perform direct investigation of the correlation between fine magnetic
structures located at loop footpoints.
Correspondence
Yukio Katsukawa (yukio.katsukawa@nao.ac.jp), National Astronomical Observatory of Japan
presentation
invited