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Modelling explosive events in the solar
L.M. Sarro, 1 R. Erd'elyi, 2 J.G. Doyle, 3 and M.E. P'erez 3
1 Laboratorio de Astrof'isica Espacial y F'isica Fundamental (LAEFF) INTA, P.O. Box 50727,
28080 Madrid, Spain, Email:email@example.com
2 Department of Applied Mathematics, University of Sheffield, Hicks Building, Western Bank,
S3 7RH, England (U.K.), Email: Robertus@sheffield.ac.uk
3 Armagh Observatory, College Hill, Armagh, BT61 9DG, N. Ireland, Email: firstname.lastname@example.org,
Received ; accepted
Abstract. High--resolution ultraviolet (UV) spectra of the outer solar atmosphere show
transient brightenings often referred to as explosive events. These are localized regions
of small spatial extent that show sudden enhancements in the intensities of lines formed
between 20,000 and 200,000 K, accompanied by strong nongaussian profiles.
The present work is an attempt to extract observational consequences from compu
tational simulations of the dynamic response of a coronal loop to energy perturbations.