Volume 380, Number 2, December III 2001
|Page(s)||719 - 726|
|Section||Planets and planetary systems|
|Published online||15 December 2001|
Modelling of solar explosive events in 2D environments
III. Observable consequences
Armagh Observatory, College Hill, Armagh, BT61 9DG, N. Ireland e-mail: firstname.lastname@example.org
2 High Altitude Observatory, NCAR, 3450 Mitchell Lane, Boulder, CO 80301, USA
3 School of Mathematics & Statistics, Univ. of St. Andrews, St. Andrews, Fife KY16 9SS e-mail: email@example.com
4 Space & Atmosphere Research Center, Univ. of Sheffield, Hounsfield Road, Sheffield, S3 7RH e-mail: Robertus@sheffield.ac.uk
Corresponding author: I. Roussev, firstname.lastname@example.org
Accepted: 25 October 2001
We examine the response via line synthesis of two representative transition region lines, namely C iv 1548.2 Å and O vi 1031.9 Å, in various physical environments representing the "quiet" Sun to magnetic reconnection events. Our calculations of ion populations allow for departures from equilibrium ionization (EI), which is critical in studies of transient events. Both lines reveal highly blue- and red-shifted Doppler components, and some of the results are examined in the context of solar explosive events. The observable consequences of magnetic reconnection are subtle in the various physical circumstances examined here and differ from one emission line to another, because of the difference in their formation temperatures.
Key words: MHD / Sun: atmosphere / Sun: chromosphere / Sun: UV radiation / Sun: magnetic fields / line: profiles
© ESO, 2001
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