Electron acceleration and transport during the November 5, 1998 solar flare at ∼13:34 UT
Tipo
Artigo
Data de publicação
2006
Periódico
Solar Physics
Citações (Scopus)
5
Autores
Trottet G.
Correia E.
Karlicky M.
Aulanier G.
Yan Y.
Kaufmann P.
Correia E.
Karlicky M.
Aulanier G.
Yan Y.
Kaufmann P.
Orientador
Título da Revista
ISSN da Revista
Título de Volume
Membros da banca
Programa
Resumo
This paper deals with a detailed analysis of spectral and imaging observations of the November 5, 1998 (Hα 1B, GOES M1.5) flare obtained over a large spectral range, i.e., from hard X-rays to radiometric wavelengths. These observations allowed us to probe electron acceleration and transport over a large range of altitudes that is to say within small-scale (a few 10 3 km) and large-scale (a few 105 km) magnetic structures. The observations combined with potential and linear force-free magnetic field extrapolations allow us to show that: (i) Flare energy release and electron acceleration are basically driven by loop-loop interactions at two independent, low lying, null points of the active region magnetic field; (ii) <300 keV hard X-ray-producing electrons are accelerated by a different process (probably DC field acceleration) than relativistic electrons that radiate the microwave emission; and (iii) although there is evidence that hard X-ray and decimetric/metric radio-emitting electrons are produced by the same accelerator, the present observations and analysis did not allow us to find a clear and direct magnetic connection between the hard X-ray emitting region and the radio-emitting sources in the middle corona. © Springer 2006.