Loop modeling of coronal X-ray spectra. I. General properties.

Details Loop modeling of coronal X-ray spectra. I. General properties. Loop modeling of coronal X-ray spectra. I. General properties.

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...306..553c&link_type=abstract

Astronomy and Astrophysics, v.306, p.553

Astronomy and Astrophysics

Astrophysics

21

Stars: Coronae, Stars: Late-Type, Plasmas, Ultraviolet: Stars, X-Rays: Stars

Scientific paper

This work is motivated by the widely accepted paradigm that the structure and features of stellar coronae are determined by plasma magnetically confined in coronal loops. In particular we address the question whether it is possible to devise diagnostics amenable to reveal some physical and geometric characteristics of static coronal loops from X-ray observations. We show that single-loop coronal models may give spectra differing in several respects from one- and two-temperature models, the differences being probably observable already with ASCA/SIS. We find that the spectra of our loop models are essentially determined by the plasma below one pressure scale height; therefore we do not need to consider deviations from Spitzer's conductivity which occur in the very diluted upper atmosphere. We also find that widening of cross section of the loops may give observable effects depending on loop parameters and that even a small fraction of the star's surface covered by compact coronal loops with dense plasma can easily dominate the emission from a corona and mask the emission from long and tenuous loops. Finally we present an example of fitting a real ROSAT/PSPC observation with loop-emitted spectra.

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