Observations of an X1.2 flare at submillimeter wavelenghts

GERMÁN CRISTIANI, CARLOS GUILLERMO GIMÉNEZ DE CASTRO, CRISTINA HEMILSE MANDRINI, MARTA GRACIELA ROVIRA, PIERRE KAUFMANN

La Plata, Pcia. de Buenos Aires, Argentina

Congreso; 48va Reunión Anual de la Asociación Argentina de Astronomía; 2005

Asociación Argentina de Astronomía

We analyze the solar event on October 30, 2004, that ocurred in active region (AR) 10691 (N13W18) at 11:38 UT. High time resolution observations at 212 GHz obtained with the Submillimeter Solar Telescope (SST) showed a very impulsive event (~1500 s.f.u.), followed by a long-lasting thermal phase. The burst was also observed at 405 GHz, the second observational frequency of SST. We combine SST data with the observations of the Radio Solar Telescope Network (RSTN) to determine the radio spectrum. This spectral analysis does not allow us to infer the presence of the THz component seen by Kaufmann et al (2004). EUV images from the Extreme Ultraviolet Imaging Telescope (SoHO/EIT) are used to identify the possible emitting sources. Assuming that the origin of the emission during the impulsive phase is gyrosynchrotron radiation from mildly relatisvistic electrons, we derive the parameters of the accelerated electrons and emitting source.