Volume 564, April 2014
|Number of page(s)||7|
|Published online||04 April 2014|
MHD modeling of coronal loops: the transition region throat ⋆
Dipartimento di Fisica & ChimicaUniversità di
Piazza del Parlamento 1,
2 now at: CINECA – Interuniversity consortium, via Magnanelli 6/3, 40033 Casalecchio di Reno, Bologna, Italy
3 INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
4 Dipartimento di Fisica Generale, Università di Torino, via Pietro Giuria 1, 10125 Torino, Italy
5 NASA Goddard Space Flight Center, Greenbelt MD 20771, USA
Accepted: 29 January 2014
Context. The expansion of coronal loops in the transition region may considerably influence the diagnostics of the plasma emission measure. The cross-sectional area of the loops is expected to depend on the temperature and pressure, and might be sensitive to the heating rate.
Aims. The approach here is to study the area response to slow changes in the coronal heating rate, and check the current interpretation in terms of steady heating models.
Methods. We study the area response with a time-dependent 2D magnetohydrodynamic (MHD) loop model, including the description of the expanding magnetic field, coronal heating and losses by thermal conduction, and radiation from optically thin plasma. We run a simulation for a loop 50 Mm long and quasi-statically heated to about 4 MK.
Results. We find that the area can change substantially with the quasi-steady heating rate, e.g., by ~40% at 0.5 MK as the loop temperature varies between 1 MK and 4 MK, and, therefore, affects the interpretation of the differential emission measure vs. temperature (DEM(T)) curves.
Key words: Sun: corona / Sun: magnetic fields / Sun: transition region / magnetohydrodynamics (MHD)
The movie associated to Fig. 4 is available in electronic form at http://www.aanda.org
© ESO, 2014
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