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A new estimation of the total number and energy of the non-thermal electronsproduced in the giant ($>\text{X}17$) solar flare on 2003 October 28 ispresented based on the analysis of the observations of the hard X-ray (HXR)emission by the High Energy Neutron Detector (HEND) onboard the Mars Odysseyspacecraft orbiting Mars. Previous estimations of the non-thermal electronenergy based on the Reuven Ramaty High-Energy Solar Spectroscopic Imager(RHESSI) data were incomplete since RHESSI missed the peak of the flareimpulsive phase. In contrast, HEND observed the whole flare. We used two modelsto estimate the energy of the non-thermal electrons: the cold thick targetmodel and the warm thick target model. We found that, depending on the modelused and the low-energy cutoff ($E_\mathrm{c}$) of the non-thermal electrons,the estimate of their total energy in the entire flare can vary from $2.3\times 10^{32}$ to $6.2 \times 10^{33}$ ergs. The lowest estimate, $2.3 \times10^{32}$ ergs, obtained within the cold thick target model and fixed$E_\mathrm{c}=43$ keV, is consistent with the previous estimate. In this case,non-thermal electrons accelerated in the peak of the flare impulsive phasemissed by RHESSI contained approximately $40\%$ of the total energy ofnon-thermal electrons of the entire flare. The highest value, $6.2 \times10^{33}$ ergs, obtained with the cold thick target model and fixed$E_\mathrm{c}=10$ keV, looks abnormally high, since it exceeds the totalnon-potential magnetic energy of the parent active region and the totalbolometric energy radiated in the flare. Our estimates also show that the totalnumber and energetics of the HXR-producing electrons in the flare region is afew orders of magnitude higher than of the population of energetic electronsinjected into interplanetary space.

New estimation of non-thermal electron energetics in the giant solar flare on 28 October 2003 based on Mars Odyssey observations