%0 Journal Article
%@issn 0273-1177
%T Highlights of the Brazilian Solar Spectroscope
%D 2009
%8 Jul.
%A Sawant, Hanumant Shakar,
%A Cecatto, José Roberto,
%A Meszarosova, Hana,
%A Faria, C.,
%A Fernandes, Francisco Carlos Rocha,
%A Karlicky, Marian,
%A Andrade, Maria Conceição,
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Repu
%@affiliation Pontificia Univ Catolica Minas Gerais, Dept Comp Sci, Pocos De Caldas, MG Brazil
%@affiliation Inst Res & Dev IP&D UNIVAP, BR-12244000 Sao Jose Dos Campos, Brazil
%@affiliation Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%B Advances in Space Research
%V 54-57
%N 1
%P 54-57
%K Sun, Instrumentation, Spectroscope, Corona, Radio radiation.
%X The digital, decimetric (950-2500 MHz) Brazilian Solar Spectroscope (BSS, Sawant, H.S., Subramanian, K.R., Faria, C., et al. Brazilian Solar Spectroscope (BSS). Solar Phys. 200, 167-176, 2001) with high time (10-1000 ms) and frequency (1-10 MHz) resolution is in regular operation since April, 1998, at the National Space Research Institute (INPE) at Sao Jose dos Campos, Brazil. The BSS has now been upgraded with a new digital data acquisition and data processing system. The new version of the BSS has improved the observational possibilities with the capability to record up to 200 frequency channels available in the selectable frequency range 950-2500 MHz. The GPS receiver permits the acquisition of data with time accuracy in the order of 0.1 ins. The software system of the BSS is composed by two distinct modules: the first, data acquisition system provides a flexible Graphical User Interface (GUI) that allows one to choose the observational parameters. The second module is the real time visualization system that permits real time visualization of the observed dynamic spectrum and additionally allows procedures for visualization and preliminary analysis of the recorded solar spectra. Using the new visualization system, we have realized two new types of dm-radio fine structures: narrow band type Ill bursts with positive as well as negative group frequency drift and dots emissions arranged in zebra-like and fiber-like chains. Furthermore, we have found flare generated fast wave trains according to their tadpole signature in wavelet power spectra for a decimetric type IV radio event (June 6, 2000 flare).
%@language en
%3 sawant.pdf