Volume 383, Number 2, FebruaryIV 2002
|653 - 660
|Planets and planetary systems
|15 February 2002
Models for solar magnetic loops
I. A simple theoretical model and diagnostic procedure
Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, Italy
2 Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany
3 Naval Research Laboratory, Washington DC, 20375-5320, USA
Corresponding author: E. Landi, firstname.lastname@example.org
Accepted: 28 November 2001
In the present paper the quasi-static model of Landini & Monsignori Fossi ([CITE]) for coronal loops is improved and a simple diagnostic procedure is developed to compare the most important physical properties of the model with a set of spectral observations of loops such as those obtained by the CDS and SUMER instruments on SOHO. The model assumes quasi-static and isobaric conditions and solves the energy equation among radiative losses, a constant heating function and heat conduction. The model is allowed to have a variable loop section. To better match the latest observational results, an isothermal section of the loop is added at the top of the loop model; its effects on the diagnostic technique and on the shape of the unknown heating function are discussed. A numerical simulation is shown and the effect of the isothermal region is discussed. In a second paper (Brković et al. [CITE], Paper II) the present model will be compared with observations from the SOHO satellite.
Key words: Sun: corona / techniques: miscellaneous
© ESO, 2002
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