EDP Sciences
Free access
Volume 502, Number 3, August II 2009
Page(s) 957 - 968
Section The Sun
DOI http://dx.doi.org/10.1051/0004-6361/200810899
Published online 15 June 2009
A&A 502, 957-968 (2009)
DOI: 10.1051/0004-6361/200810899

Analytical model of static coronal loops

J. Dudík1, E. Dzifčáková1, 2, M. Karlický2, and A. Kulinová1, 2

1  Department of Astronomy, Physics of the Earth and Meteorology, Faculty of Mathematics, Physics and Informatics, Comenius University, Mlynská Dolina F2, 842 48 Bratislava, Slovak Republic
    e-mail: dudik@fmph.uniba.sk
2  Astronomical Institute of the Academy of Sciences of the Czech Republic, Fričova 298, 251 65 Ondřejov, Czech Republic

Received 9 September 2008 / Accepted 23 March 2009

By solving the energy-equilibrium equation in the stationary case, we derive analytical formulae in the form of scaling laws for non-uniformly heated and gravitationally stratified coronal loops. The heating is assumed to be localized in the chromosphere and to exponentially decrease with increasing distance along the loop strand. This exponential behavior of the heating and pressure profiles implies that we need to use the mean-value theorem, and in turn fit the mean-value parameters of the scaling laws to the results of the numerical simulations. The radiative-loss function is approximated by a power-law function of the temperature, and its effect on the resulting scaling laws for coronal loops is studied. We find that this effect is more important than the effect of varying loop geometry. We also find that the difference in lengths of the different loop strands in a loop with expanding cross-section does not produce differences in the EUV emission of these strands significant enough to explain the observed narrowness of the coronal loops.

Key words: hydrodynamics -- Sun: corona -- Sun: UV radiation -- stars: coronae

© ESO 2009