  A new estimation of the total number and energy of the non-thermal electrons
produced in the giant ($>\text{X}17$) solar flare on 2003 October 28 is
presented based on the analysis of the observations of the hard X-ray (HXR)
emission by the High Energy Neutron Detector (HEND) onboard the Mars Odyssey
spacecraft orbiting Mars. Previous estimations of the non-thermal electron
energy based on the Reuven Ramaty High-Energy Solar Spectroscopic Imager
(RHESSI) data were incomplete since RHESSI missed the peak of the flare
impulsive phase. In contrast, HEND observed the whole flare. We used two models
to estimate the energy of the non-thermal electrons: the cold thick target
model and the warm thick target model. We found that, depending on the model
used 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, $2.3 \times
10^{32}$ 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 phase
missed by RHESSI contained approximately $40\%$ of the total energy of
non-thermal electrons of the entire flare. The highest value, $6.2 \times
10^{33}$ ergs, obtained with the cold thick target model and fixed
$E_\mathrm{c}=10$ keV, looks abnormally high, since it exceeds the total
non-potential magnetic energy of the parent active region and the total
bolometric energy radiated in the flare. Our estimates also show that the total
number and energetics of the HXR-producing electrons in the flare region is a
few orders of magnitude higher than of the population of energetic electrons
injected into interplanetary space.
