Luís Olavo de Toledo Fernandes, Mr. - MSc
Centro de Rádio Astronomia Astrofísica Mackenzie, Escola de Engenharia, Universidade Presbiteriana Mackenzie, São Paulo, SP, Brasil
       
       
Session 1 - Poster

Solar flare observations at 30 THz
R. Miteva (Space Research and Technology Institute, Bulgarian Academy of Sciences, Bulgaria and CRAAM/MPU, Brazil), P. Kaufmann (CRAAM/MPU and State University of Campinas, Brazil), D. P. Cabezas (CRAAM/MPU, Brazil), M. M. Cassiano (CRAAM/MPU, Brazil), L. O. T. Fernandes (CRAAM/MPU, Brazil), S. L. Freeland (Lockheed Martin Solar and Astrophysics Laboratory, USA), M. Karlicky (Astronomical Institute of the Academy of Sciences of the Czech Republic), A. Kerdraon (LESIA-Observatoire de Paris, France), A. S. Kudaka (CRAAM/MPU, Brazil), M. L. Luoni (Institute of Astronomy and space Physics, CONICET/UBA, Argentina), R. Marcon (State University of Campinas and Bernard Lyot Solar Observatory Campinas, Brazil), J.-P. Raulin (CRAAM/MPU, Brazil), G. Trottet (LESIA-Observatoire de Paris, Meudon), S. M. White (Air Force Research Laboratories, Space Vehicles Directorate, USA)
       

We report the detection of an intense 30 THz impulsive burst on 1 August 2014 with the equipment installed at the Center of Radio Astronomy and Astrophysics (CRAAM) in Mackenzie Presbyterian University (MPU), Sao Paulo, Brazil. The event is associated with a GOES M2 class solar flare. The maximum flux at 30 THz was about 19000 sfu, almost two orders of magnitude larger than measured at microwave frequencies. The microwave emissions at higher frequencies exhibit a suggestive time association with the 30 THz peak. At the metric-to-decimetric frequency range a superimposed short duration burst occurs close to the peak of the 30 THz emission while the underlying slower emission maximum is progressively delayed for lower frequencies. The dynamic radio spectrum shows signatures of drifting pulsations and reversed type III-like radio bursts. No emissions in white light or sub-millimeter wavelengths were detected. Hard X-rays produced by the event was partially observed by the FERMI satellite only at the beginning, because the satellite was eclipsed by the terrestrial atmosphere. A good correspondence between the temporal profiles and positions at 30 THz, EUV and H-alpha wavelengths was observed. The flaring source seen at EUV and H-alpha has finer spatial structures not resolved within the 30 THz 15 arc-seconds photometric beam. It is suggested that the 30 THz, EUV and H-alpha brightening originate from a common flaring site at the low chromosphere. A comparative analysis with the first reported 30 THz burst on 13 March 2012 is presented.