@Article{CuambeCostSimõ:2018:FlPaIn,
               author = "Cuambe, Valente A. and Costa, Joaquim Eduardo Rezende and 
                         Sim{\~o}es, P. J. A.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {University of 
                         Glasgow}",
                title = "Flare parameters inferred from a 3D loop model data base",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2018",
               volume = "477",
                pages = "1508--1519",
                month = "June",
             keywords = "Sun: activity, Sun: flares, Sun: magnetic field, Sun: radio 
                         radiation.",
             abstract = "We developed a data base of pre-calculated flare images and 
                         spectra exploring a set of parameters which describe the physical 
                         characteristics of coronal loops and accelerated electron 
                         distribution. Due to the large number of parameters involved in 
                         describing the geometry and the flaring atmosphere in the model 
                         used, we built a large data base of models (similar to 250 000) to 
                         facilitate the flare analysis. The geometry and characteristics of 
                         non-thermal electrons are defined on a discrete grid with spatial 
                         resolution greater than 4 arcsec. The data base was constructed 
                         based on general properties of known solar flares and convolved 
                         with instrumental resolution to replicate the observations from 
                         the Nobeyama radio polarimeter spectra and Nobeyama 
                         radioheliograph (NoRH) brightness maps. Observed spectra and 
                         brightness distribution maps are easily compared with the modelled 
                         spectra and images in the data base, indicating a possible range 
                         of solutions. The parameter search efficiency in this finite data 
                         base is discussed. 8 out of 10 parameters analysed for 1000 
                         simulated flare searches were recovered with a relative error of 
                         less than 20 per cent on average. In addition, from the analysis 
                         of the observed correlation between NoRH flare sizes and 
                         intensities at 17 GHz, some statistical properties were derived. 
                         From these statistics, the energy spectral index was found to be 
                         delta similar to 3, with non-thermal electron densities showing a 
                         peak distribution less than or similar to 10(7) cm(-3), and 
                         B-photosphere greater than or similar to 2000 G. Some bias for 
                         larger loops with heights as great as similar to 2.6 x 10(9) cm, 
                         and looptop events were noted. An excellent match of the spectrum 
                         and the brightness distribution at 17 and 34 GHz of the 2002 May 
                         31 flare is presented as well.",
                  doi = "10.1093/mnras/sty867",
                  url = "http://dx.doi.org/10.1093/mnras/sty867",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "cuambe_flare.pdf",
        urlaccessdate = "18 abr. 2024"
}