MODELADO DEL CAMPO MAGNÉTICO SOLAR Y SU RELACIÓN CON OBSERVACIONES EN ULTRAVIOLETA Y RAYOS X DURANTE UNA FULGURACIÓN SOLAR

Autores/as

  • L. G. Bagalá Instituto de Astronomía y Física del Espacio (CONICET), Universidad Nacional de Buenos Aires.
  • C. H. Mandrini Instituto de Astronomía y Física del Espacio (CONICET), Universidad Nacional de Buenos Aires.
  • M. G. Rovira Instituto de Astronomía y Física del Espacio (CONICET), Universidad Nacional de Buenos Aires.
  • P. Démoulin Observatoire de París.

Resumen

The longitudinal magnetic field of solar active region, observed on the solar disk during November 1980, is modelled by means of a distribution of subphotospheric discrete sources in the potencial and linear force-free approach. The topological structure derived from these models is compared with the location of 4 brightenings due to a solar flare. These kernels are identified in the UV and X-rays images obtained by two instruments that flew aboard the Solar Maximum Mission Satellite. The identified brightenings are located at the intersection of the separatrices with the photospheric plane and can be connected by field lines passing close to the separator.

This indicates that this flare can be the result of the interaction through magnetic field reconection of two or more structures in the separator region.

Biografía del autor/a

P. Démoulin, Observatoire de París.

París, France.

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Publicado

2013-08-30

Número

Vol. 5 Núm. 1 (1994): ANALES AFA - Volumen 5 No 1 - Rosario

Sección

Física del Espacio y del Ambiente. Geofísica