All Tables

Table 1: Effective areas and transmission factors of the SPI gamma-ray camera for the observation conditions of the flare obtained by MGGPOD simulations with a detailed model of SPI and the spacecraft.
Table 2: Results of the spectrum fits for the three strongest lines and the underlying continuum. Line centroids and $\sigma$ are in keV, rates are dead-time corrected counts/s and line fluences are expressed in photons/cm². S is the power-law index of the observed photon spectrum. Error bars result from the fit with an additional uncertainty of 10% for the fluences, due to an uncertainty on the effective area, added quadratically to the error bar of the fit.
Table 3: Results of separate fits to the ¹²C-line at 4.4 MeV and the ¹⁶O-line line at 6.1 MeV assuming a thick-target interaction model and three different energetic particle angular distributions around the flare axis. Rates and fluences are expressed as in table I. Error bars on count rates encompass the individual 1-sigma uncertainties of the different fits; a 10% uncertainty has been quadratically added to the error bars of line fluences.
Table 4: Best fit values of angular distribution width parameter $\Delta \Theta$ for DW flares and of $\alpha$ /p for DW and PAS( $\lambda =30$ ) flares for combined fits of the ¹²C and ¹⁶O lines. Spectral index of accelerated particles s=4.0; values in parenthesis are for s=3.0. The values of $\alpha$ /p and $\Delta \Theta$ for s=3.5 are generally between those of s=3.0 and s=4.0.