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Multi-wavelength investigation of energy release and transport in the 16 August 2004 flare

Published online by Cambridge University Press:  01 September 2007

L. K. Kashapova
Affiliation:
Radioastrophysical Department, Institute of Solar-Terrestrial Physics, Irkutsk, Russia email: lkk;grechnev@iszf.irk.ru
V. V. Zharkova
Affiliation:
Department of Computing and Mathematics, University of Bradford, Bradford, UK email: v.v.zharkova@Bradford.ac.uk
V. V. Grechnev
Affiliation:
Radioastrophysical Department, Institute of Solar-Terrestrial Physics, Irkutsk, Russia email: lkk;grechnev@iszf.irk.ru
S. S. Ipson
Affiliation:
Department of Electronic Imaging and Media Communication, University of Bradford, Bradford, UK email: s.s.ipson@Bradford.ac.uk
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Abstract

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The current contribution investigates the solar flare of 16th August 2004 with the multi-wavelength observations with high temporal resolution from RHESSI, Large Solar Vacuum Telescope (LSVT), Hiraiso Solar observatory, Nobeyama Radioheliograph (NoRH, 17 and 34 GHz) and Siberian Solar Radio Telescope (SSRT, 5.7 GHz), TRACE. The main flare was preceded by a pre-flare event with a very short energy release time. The observations of the main flare reveal a close temporal correlation between the Hα intensity observed with LSVT and those in hard and soft X-ray emissions observed with RHESSI, and in microwave fluxes observed with NoRH and SSRT. This close temporal correlation can be only associated with high-energy particles. The role of energetic particles in energy transport and non-thermal excitation and ionisation on Hα emission during the pre-flare and pre-flare event is investigated with full non-LTE approach and possible agents and scenarios of energy transport are discussed.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Dalla, S. & Browning, P., 2005, A A, 436, 1103.CrossRefGoogle Scholar
Grechnev, V.V. et al. , 2003, Solar Phys. 216, 239.CrossRefGoogle Scholar
Handy, B. N., et al. , 1999, Solar Phys., 187, 229.CrossRefGoogle Scholar
Lin, R. P., et al. , 2002, Solar Phys., 210, 3.CrossRefGoogle Scholar
Nakajima, et al. , 1994, “The Nobeyama Radioheliograph”, Proc. of the IEEE, 82, 705.CrossRefGoogle Scholar
Scherrer, P. H., et al. , 1995, Solar Phys. 162, 129.CrossRefGoogle Scholar
Skomorovsky, V.I. & Firstova, N.M., 1996, Sol. Phys., 163, 209.CrossRefGoogle Scholar
Zharkova, V.V. & Gordovskyy, M., 2004, Astrophys.J, 604, 884.CrossRefGoogle Scholar
Zharkova, V.V., Zharkov, S.I., Ipson, S.S. and Benkhalil, , 2005, JGR., 110 N A8, doi:10.1029/2004JA010934, p.104-128.CrossRefGoogle Scholar
Zharkova, V.V. & Gordovskyy, M., 2005, MNRAS, 356, 1107.CrossRefGoogle Scholar