We study an event which occurred in NOAA 8471, where an M6.6 flare and the activation of two filaments were observed on 28 February 1999. A multi-wavelength study allows us to investigate the behavior of the several features observed at different atmospheric levels, that might be used to answer to the question whether and in what conditions the eruption of filaments can play an active or a passive role in the flare occurrence. Imaging data were acquired by BBSO in the Halpha line and by TRACE in the 1216, 1600, 171 and 195 Å channels, allowing us to deduce the morphology and temporal evolution of the event and to estimate the Ly-alpha power. Moreover, in order to study the magnetic topology, the extrapolation of the photospheric magnetic field lines was done assuming potential field and using SOHO/MDI magnetograms.
Relationship between an M6.6 solar flare and subsequent filament activations.
RUBIO DA COSTA, FATIMA;Zuccarello F;Romano P.;
2012-01-01
Abstract
We study an event which occurred in NOAA 8471, where an M6.6 flare and the activation of two filaments were observed on 28 February 1999. A multi-wavelength study allows us to investigate the behavior of the several features observed at different atmospheric levels, that might be used to answer to the question whether and in what conditions the eruption of filaments can play an active or a passive role in the flare occurrence. Imaging data were acquired by BBSO in the Halpha line and by TRACE in the 1216, 1600, 171 and 195 Å channels, allowing us to deduce the morphology and temporal evolution of the event and to estimate the Ly-alpha power. Moreover, in order to study the magnetic topology, the extrapolation of the photospheric magnetic field lines was done assuming potential field and using SOHO/MDI magnetograms.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
